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THE CHARACTERISTICS AID :MOTIONS OF JUPITER'S SPOTS
DURING A OE-YEAiR PERIOD
by.
Olark R.
Chapman
A.B. Harvard University
(1967)
SUB1ITTED ~T PARTIAL FULFILUM-ET
OF THE REQUIRERINTTS FOR THE
DEGREE OF MASTER OF
SCIEMICE
at the
MASSACHUSETTS IHSTITUTE OF
TE SjHOLOGY
Setermber,
1968
Siznature of
Department of Meteorology,
Certified by.....
..
August 19,
...........................
1968
............
..
Thesis Supervisor
Accepted
by
..
.....
0.
Chairman,
a
S..9
*0,
......
******
Departmental Committee on Graduate Students
Lind
1
SEPFIQ
1
'~
.a~a~el;::r.~-i~: r:,
B;drt1PW*1
ES
THE CHARACTERISTICS A:D TMOTIO: OF JUPITER'S SPOTS
DURING A OE-YEAR PERIOD
Clark R. Chapman
Submitted to the Department of Meteorology on August 19, 1968, in partial
fulfillment of the requirement for the degree of Master of Science.
Abstract -- The statistics of the spots in the belts of the planet Jupiter have been studied in the past only by visual observations. This report presents the results of the first phase of a pilot project utilizing
the photographic patrol plates taken at the New Mexico State University
Observatory. The beginning sections describe the earlier observing methods
and summarize the characteristics of Jupiter's spots and zonal currents
determined from the earlier techniques.
There follows a description of the N.M.S.U. plate collection and
the methods used to order the photographic data into useable form. Nine
synoptical photographic drift charts, showing the evolution of Jupiter's.
spots in nine zonal regions during the 1968-7 apparition, were constructed
and data were taken concerning spot motions, shapes, sizes, lifetimes, etc.
A computer was used to determine numerous characteristics of the spot
populations in the individual currents and relationships between spot
parameters. The resulting lists of observed spots form the first reasonably objective and uniform data. sample on Jupiter's spots and the derived
statistics and relationships form a source for comparison with theoretical
Numerical results are presented herein
models for Jupiter's circulation.
covering Jupiter's entire northern hemisphere, with the exception of the
equatorial jet, for the period November 198 through November 1987 (but
June to INovember 1967 is poorly covered because Jupiter was near solar
conjunction).
The region of zonal shear bordering the equatorial jet is
characterized by highly variable spot velocities and by shorter spot lifetimes. Unfortunately, lifetimes can be determined reliably for only a
minority of spots, even in stable currents, and the apparent absence of
strong correlation between size and lifetime requires further study.
Small spots and dark spots may rotate more rapidly than large or light 0
spots in some latitudes. The apparent preferred length for spots of 5
nay simply reflect loss of completeness of smaller spots; latitudinal
widths of spots, generally about three-quarters of spot lengths are less
variable than spot lengths. Many of the other potential correlations
between spot parameters were found to be-weak or absent. Tabulations of
all observed spots and summaries of the findings concerning spot characteristics are presented in extensive appendices.
TABet -0F C00ITENTSf
I.
Introduction
5
II.
Previous Studies of Jupiter's Spots
9
A.
Observing methods
10
B.
Reductions of amateur data
13
.0. Characteristics of Jupiter.'s circulation -results
III.
18
The Methods Used for Obtaining Data on Jupiter's Spots
from the Photographic Patrol
21
A.
Construction of photographic drift charts
21
The patrol photographs
21
The photographic prints
23
Reduction of srot statistics from the drift charts
29
Tracing spots on overlays
29
Measured information about the spots
31
B.
IV.
early
Computer Analysis of the Characteristics of Jovian Spots
and Currents
36
A.
Spot characteristics
38
Definite, probable, and possible spots
36
Spot lifetimes
38
Spot motions
40
Spot lengths
41
B.
Characteristics of currents
42
C.
Relationships between spot characteristics
43
D.
Size-lifetime relationships
44
V.
Summary of conclusions
VI.
Acknowl ed gem ents
49
VII.
References
50
VIII.
Appendices
51
A.
Characteristics of currents
53
B.
Tabulations of all observed spots
68
0.
Relationships between spot characteristics
115
D.
Lifetime-size relationships
128
I. I1NTROD OTION
The planet Jupiter is less that a minute of arc in diameter as
seen from the Earth.
Nevertheless the gross pattern of the general cir-
culation of the planet's atmosphere (at the height of the presumed "tropopause") has been ascertained to a degree not greatly inferior to our knowledge of the general pattern of the terrestrial circulation, at least until
recent times.
Indeed the oblateness of the planet,
due to its
rapid rota-
tion, and the zonal cloud belts were recognized over three centuries ago,
shortly after the invention of the telescope.
In 1685 J.D.
Cassini dis-
covered a large South Tropical spot (probably the Great Red Spot; see Chapman,
1968a)
and determined its
rotation period.
In
subsequent years, Cas-
sini measured changes in the motion of the Red Spot and also discovered the
considerably more rapid motion of spots in
equatorial latitudes (the equa-
torial acceleration).
Beginning about a century ago, amateur astronomers from many
countries, but notably England, began to observe Jupiter regularly and to
issue systematic summaries about the planet's telescopic appearance and the
motions of spots in several well-defined zonal currents, based on visual
timings of spot transits across Jupiter's central meridian.
Such records
through 1948 have been summarized by B.M. Peek (1958) in his comprehensive
boock, The Planet Jupiter.
Despite the magnitude of the accumulated data from amateur astronomers' observations, far less has been learned from such observations
5
than is
possible using modern techniques.
First, the visual observations
of Jupiter suffer from their subjectivity and human errors.
data sample is
Secondly, the
highly heterogeneous and the data reductions to date have
been quite simple and in many ways incomplete and inadequate.
The advan-
tages' and limitations of the past visual work are discussed in
detail later.
Since the initiation-of the first regular photographic patrol of
Jupiter.
now in about its
sixth year at the New Mexico State University
Observatory in Las Cruces, there is for the first time a large, uniform,
objective record of Jupiter which is of sufficient quality to enable many
kinds of investigations never before possible to be carried out with relative ease.
The present report discusses an early phase of the first com-
prehensive analysis of a portion of the New Mexico photographic records.
The study is an outgrowth of an original investigation planned
by Prof. Raymond Hide and the present author of the relationship between
size, and lifetimes of Jupiter's spots.
In order to investigate one part
of the lifetime spectrum (a few days to a year),
a seriies of photogr'aphic
charts were constructed from the New Mexico plates,
an orderly fashion (to be discussed in
designed to display in
detail later on) synoptical pictures
of Jupiter covering one apparition of the planet.
(An apparition is a per-
iod of about 13 months measured from one solar conjunction to the next.)
However,
the charts provide a ready source of information on 7any other
characteristics
of Jupiter's spots and its
and lifetimes.
The present analysis is
currents than just the sizes
an attempt to learn.about many as-
pects of Jupiter's visible atmospheric surface from these charts.
The intent is to derive empirical information concerning many
characteristics of spots (including si7e, color, shape, motions, location,
characteric
ofsosi
etc.) and on the characteristics of the zonal currents.
Some kinds of
information which are gleaned from the charts simply refine. cruder work
already accomplished by amateur astronomers for the same period (e.g.
Budine, 1968),
Other characteristics which are investigated were suggested
by terrestrial analogues with meteorological implications.
Still other
characteristics investigated are intended to be useful in other projects
currently under way (for instance the size-lifetime study of Prof. Hide;
also the study of momentum transfer in the Jovian atmosphere by Prof.
Victor Starr and his collaborators).
The scope of this report is a limited one.
By no means is it
intended to be the last word on the characteristics of Jupiter's visible
surface features.
Rather, it is intended to be the preliminary first step
in the objective analysis of Jupiter patrol photographs --
a pilot study.
The coverage could be extended considerably now that several more years of
patrol photographs have been taken, and better more automated techniques
for analysing the photographic images are being devised (for instance by
Starr's group).
Some of the kinds of information and correlations devel-
oped here will justify further study in the future, while still other kinds
of analysis can and will be nerformed using the present charts.
There is
no attempt in
this thesis to nut forward physical hy-
potheses to help "explain" the relationships which apnesr.
too premature to do so.
It would be far
Our knowledge of the physical nature of the belts
and spots under investigation is
so rudimentary thLt the first
be to lay the epnnirical foundations.
task must
It is the purpose of this thesis (to-
gether with the already extant and long-term, though cruder, records of
amateur astronomers)
to form this empirical foundation.
7
Further development in several directions is planned.
The pre-
liminary data on the size-lifetime relationship presented herein will be
amplified upon and presented, together with data -on more long-lived spots
and with a preliminary theoretical interpretation, in a report currently in
preparation (Hide and Chapman, 1968).
The present studies of the spot and
current motions will serve as the basis from which the more sophisticated
technic ues of Starr et al will be developed in
a theoretical-empirical
study of the dynamical processes of Jupiter's general circulation.
paper is
Another
planned which will use the present study as a basis for suggesting
improvements in the traditional methods which amateur astronomers have been
using for studying Jupiter; it
appears likely that amateur data will be the
primary source for much of our information about Jupiter's snots for some
years to come.
Many of the characteristics of Jupiter's appearance and circulation appear to vary from year to year, but the present study considers only
a relatively brief segment of time.
Therefore,
to establish the context of
of the present results, it is necessary first to discuss the previous work
by amateur astronomers -able detail.
both the results and the methods --
This is the purpose of Section II.
in consider-
Section III then de-
scribes the techniques for obtaining the data used in the present study.
The results, mainly tabular in nature, are presented in Section IV.
imnlications of the results are discussed in the concluding section.
8
Some
II.
PREVIOUS STUDIES OF JUPITER'S SPOTS
Telescopic observations by amateur and semi-professional astronomers form the basis for m-Iost of our knowledge about the motions and characteristics of Jupiter's spots and currents.
Through a telescope, Jupiter
presents an elliptical disk about 40 seconds of arc in diameter.
Lying
parallel to the equator is a series of bright "zones" and dark "belts",
the most prominent of which are in sub-tropical latitudes.
Although these
belts and zones vary in both darkness and width, and slightly in latitude,
the major ones seem to have maintained their identity
first studied in the 1600's.
since Jupiter was
Thus a standard nomenclature has developed;
for instance from equator southward: Equatorial Band,
Equatorial Zone
(south portion), South Equatorial Belt (north component), South Equatorial
Belt Zone, South Equatorial Belt (south component), South Tropical Zone,
South Temperate Belt, South Temperate Zone, SouthwSouth Temperate Belt,
South-South Temperate Zone, South-South-South Temperate Belt, and so on,
with a similar nomenclature north of the equator.
Cassini's observations in the late 17th century provided the
first evidence for the most important characteristic of Jupiter's circulation: the 5-minute shorter rotation period for sPots within 10
equator compared with the
tude snots.
9h 5 5
m
of the
rotation period typical for higher lati-
More recently about 20 distinct zonal currents have been rec-
ognized which are more or less, but not exactly, correlated with the visible belts and zones.
The chEracteristics of these currents are described
9
following a discussion of telescopic observing methods.
A. Observing Methods
The typical telescope which has been used during the past century
for accumulating data on Jupiter is between 4
frequently a portable backyard reflector.
.nd 12 inches in aperture,
(Occasionally large professional
observatories have been used; sometimes small telescopes have been used for
observing the largest spots.)
Observers have been of all ages from early
teens up and of many nationalities.
In experience,
reliability, and dedi-
cation, observers have ranged from the very able to the very casual.
general,
In
however, most of the published reports are based largely on the
extensive work by just a few devoted and experienced American and British
observers who overwhelm the far larger number of more casual observers by
the sheer quantity of their observations.
For about 3 months centered on solar conjunctions, Jupiter is
quite unobservable.
During the next several months, it is visible only
in early morning hours when few observers can find the enthusiasm to make
regular observations.
Near times of solar opnosition, the planet is
the horizon all night
and many more observations are made --
evening.
As Jupiter again approaches conjunction,
the evenings
twilight.
and usually is- well-observed until it
above
mainly in
the
it is visible only in
is
Not all apparitions are equally favorable.
but particularly,for those in high latitudes such as in
lost in
the glare-of
For most observers,
England,
Jupiter's
12-year cyclical journey through the zodiac is crucial, and not just because of seasonal differences in the observing climate.
in
•
Gemini,
it
can rise higher than 6O0 in
10
1hen Jupiter is
the sky over -England, and remain
above the horizon for over 15 hours.
But 6 years later, when it is in
Sagittarius, Jupiter never attains 200 and even then swiftly sinks below
the horizon again.
Since the small-scale turbulence in the terrestrial
atmosphere ("seeing"),.which is so important for resolving spots in Jupiter's image, is a strong function of zenith angle (mainly due to increased
airmass), it is very difficult to obtain good observations from England
during those years when Jupiter is in the southern constellations of the
zodiac.
It is important to recognize that these and other factors strongly
affect the uniformity of Jupiter observations; for instance, the similarity
between Jupiter's zodiacal period and the sunspot cycle renders uncertain
apparent correlations between the solar cycle and Jovian phenomena.
About four chief kinds of visual observations of Jupiter have
been made during the past century with some uniformity: drawings, descriptive notes and photometry, latitude measurements, and central meridian
We will be concerned chiefly with, the last kind of observation
transits.
which yields information on longitudinal (zonal) motions of spots.
Drawings.
Hundreds of pencil sketches of Jupiter are made each
They are drawn in 10 to 20 minutes (before significant rota-
apparition.
tion has taken place) on blank disks of Jupiter's ellipticity.
eye is a more versatile detector than the camera,
The human
chiefly because it can
perceive small features during occasional brief intervals of good seeing;
photographs are usually taken at random intervals, and in any case they
integrate the image over the exposure duration (usually a fraction of a second to a couple seconds).
ist
But although drawings by an able, accurate art-
are superior to photographs in
some ways (especially in
they rarely turn out that way in practise.
small spots),
resolution of
Mary drawings
fail because of subjectivity or carelessness, frequently on the part of
.
$I
11
I
inexperienced observers.
However, prior to the recent establishment of a
photographic patrol, good photographs were not generally taken at sufficiently frequent intervals to form nearly as complete a record of Jupiter's
appearance as that formed by the multitude of sketches.
Fortunately,
studies show (e.g. Chapman, 1932) that when data taken from drawings made
by reliable observers are corrected for each observer's systematic positional errors, surprisingly high precision can be obtained from drawings
(1-o
in latitude, 2
disk).
in longitude are typical errors at the center of the
Iowever, drawings almost never have been analysed in an orderly
fashion and hence are not a source for reduced information about Jupiter.
Descrintive notes.
Amateur astronomers frecuetly write descrip-
tions of the planet each evening, including estimates of the color and relative conspicuousness of the belts and zones, as well as coments on noteworthy spots and suspected changes from previous days.
Sometimes attempts
are made to estimate the relative brightnesses of surface features on a
numerical scale; these estimates could be calibrated to yield useful -hotometric data, but never have been in practise.
Latitude measurements.
With rare exceptions, measurements of
latitudes have been restricted to the latitudes of the edges of the belts
and zones so little data is available on individual spots.
Micrometers
were often used for these measurements, but more recently measurements from
occasional photographs have usually sufficed for this purpose.
Central meridian (014) trarsits.
Probably the most useful data
to nlanetary science assembled by amateur astronomers is information obtained on the longitudes of Jovian spots from several million timings of
passages of spots across the central meridian of the planet.
The observing
procedure is quite simple: the observer merely estimates to the nearest
12
.U.~!-*
minute the time at which each spot visible rotates across the vertical
meridian bisecting the illuminated disk of Jupiter.
The observer records
each such timing along with a brief description of the spot (usually limited to its approximate latitude, relative to one of the visible belts,
and whether it
is
bright or dark).
The longitudes of the spots are then
an ephemeris such as the American
quickly determined from CGM tables in
Ephemeris and Nautical Almanac (AETA).
Longitudes are determined relative
to one of two longitude systems rotating with arbitrary periods which approximate the periods for equatorial
higher latitude periods (System II,
spots (System I,
9
h5 d
40
9 h5 0m 3 0.003s)
or the
. 6 3 2 s)@
Longitudes determined from CM transits are subject to several
systematic errors.
First, different observers show differing susceptibil-
ities to "phase exaggeration" which yields a systematic longitudinal bias
that varies with the sun-Jupiter-earth phase angle..
Secondly,
observers
have their own personal high or low biasps, which may or may not be stable
with time.
Both kinds of systematic biases can amount to more than 20 of
longitude.
Reese (1962) has shown that the accidental error in longitude
(after correction for biases) is less than 10 for a good observer.
Unfor-
tunately, 014 transits are rarely corrected for systematic errors in
pub-
lished reductions.
B.
Reductions of Amateur Data
Published reductions of CM transit data by such organizations
as the Association of Lunar and Planetary Observers and the British Astronomical Association are usually based on several thousand CM transits submitted by several dozen different observers during the course of an appari-
13
tion.
The Jupiter Directors who have performed the reductions are intel-
ligent and competent, but as unpaid amateur astronomers they have usually
lacked the time to obtain more than the bare essentials from the data.
This is all the more unfortunate now since much of the original data has
been lost or thrown away.
The method of reduction is as follows.
From exnerience, the
typical latitudinal extents of the several zonal currents are known,
a separate graph can be made for each current.
so
All CM transit longitudes
for the particular current (horizontal axis) are plotted against date,(increasing downwards),
using different symbols to distinguish dark spots
from white ones and timings of the preceding or following ends from those
of the centers.
The prominent well-observed spots are immediately ident-
ifiable on such a graph as a string of points, perhaps slenting to the
right or left depending upon whether the spot is
moving more slowly or
more rapidly than the adopted longitude system.
Lines are drawn to con--
nect the Doints for the identified spots. The identification of the more
inconspicuous or transient spots is more uncertain.
There is the danger
of connecting several points which do not refer to the same atmospheric
feature.
The determination of whether several points do represent a sin-
gle feature rests on a number of factors: the closeness of fit to a
straight drift line (indicztive of a uniform rotation peiiod), the similvrity of the apparent rate of drift to other spots in the same latitude,
and the lack of possible ambiguity in connecting soots over a long observComparisons of independent reductions of transit data during
ational gap.
the same apnrition suggest that overly optimistic identifications have
frequently been made.
Bias is undoubtedly introduced by the subjectivity
of this kind of decision-making.
~
.
a
The published reports' usually contain the following information
for each identified features dates and longitudes when first
and last re-
corded, the mean longitudinal drift per 30 days, and the corresponding rotation period.
There is occasionally a brief description of the spot be-
yond the simple designation of dark or bright.
Mean drifts, and hence
mean rotation periods, are obtained for each current,
usually unweighted
averages of the drifts of all spots deemed to be in the current.
Without belittling these valuable reports, or their general reliability, it is nevertheless worth noting that ideally far more could
have been done, and still can be done for future apnaritions and even for
past ones for which the original data still
exists.
For instance,
in
re-
cent years largely independent reports have been issued by groups in many
different countries,
including the United States, Japan, England,
Switzer-
land, Italy, and others.
It is unfortunate that attempts to pool all the
data have so far failed.
Secondly, few attempts have been made to elim-
inate observations by unreliable observers, to weight or interpret data
to take into account differing telescopes or seeing conditions, to determine and correct for personal systematic errors, or to use standard statistical procedures for determining the reliability of spot identifications.
or no attempt to use other kinds of
Thirdly, there has been little
data (such as drawings,
existing photographs,
junction with the transit data.
or written notes) in
con-
For instance, since spots occur in many
different shapes and sizes which are often stable, checking photographs or
drawings could improve the reliability of spot identifications; they could
even be used to fill
in
gaps in the GCM transit coverage.
Finally, the
many other important characteristics of spot motions besides the average
motion are lost, except in those relatively infrequent cases when the
15
original drift charts have been published.
I should repeat that to perform the kind of improved analysis
suggested above would take much more time than even the most devoted amateur astronomer could volunteer; in fact, it would take more time than
Nevertheless,
the analysis of the photographs reported on in this thesis.
it may well prove desirable to perform such reductions on a pooled collection of amateur Jupiter observations plus existing photographs for apparitions prior to the establishment of photographic patrols.
I expect such
analyses could approximate the accuracy of the present preliminary reduction of the patrol photographs.
C. Characteristics of Juniter's Circulation --
Early Results
The results of amateur astronomers' observations of the motions
of Jupiter's spots have been published in numerous reports and journals
during the past century, some of them available in observatory libraries,
but most of them small, sometimes mimeographed, publications of limited
distribution.
Perhaps the chief sources for reduced Jupiter data covering
the period 1891 to 1948 are the regular, orderly, and complete reports of
the Jupiter Section of the British Astronomical Association issued until
1943 as Memoirs of the British Astronomical Association and thereafter as
revorts in the Journal of the B. A. A.
An excellent summary of these ob-
servations has been given wide distribution as the book, The Planet Jupi;ter by B. M. Peek; however, the original renorts should be consulted for
serious investigation of past .ork.
For apparitions since 1948, a super-
ior source for Jupiter rotation data are the usually regular reports of
16
the Jupiter Section of the Association of Lunar and Planetary Observers,
published in the Journal of the Association ("The Strolling Astronomer").
These reports, prepared until recently by Mr.
Elmer J. Reese, are of cx-
ceptional quality.
I now describe what. I.feel are'the pertinent characteristics of
Jupiter's motions based on my familiarity with the literature and on sev'
eral unpublished analyses I have made based on the above sources.
Compar-
isons of independent reductions of snot data suggest that the published
tables generally provide a reliable picture of the characteristics of
Jupiter's circulation, even though misidentifications occur.
The mean
rotation period for a single spot can usually be determined to better than
1 second, althbugh spot motions frequently fluctuate about the mean by a
second or more.
If
one plots mean rotation period versus Jovian latitude, the
most obvious feature is
the equatorial acceleration: within a degree or
two of both +100 and -100,
spots switch from a rotation period similar to
that of most higher latitude spots of about 9h55 m to a period of about 9 h
5 0 1m,
which is characteristic (usually to within ( ) of snots at all lati-
tudes between + and -100
.
The non-equatorial regions of the planet do not
rotate exactly as a solid, .even in the long-term average (Chapman, 1968b).
The two hemispheres are not symetric.
in south temperate latitudes (about
both ooleward and equatorward.
The shortest average periods are
9 h 5 5 m),
with somewhat longer periods
The longest average periods are in north
temperate latitudes, with shorter periods both equatorward and poleward.
In addition to this average pattern are two well-defined latitudes of
transient, semi-periodic anomalous periods: the lonest occur in south
17
4,
sub-tropical latitudes (about 9h58m during the South Equatorial Belt disturbance) and the shortest in north sub-tropical latitudes (arourid
h 4 9 ).
9
Superimposed on this general picture are both spatial and temporal fluctuations.
I now define the word "current" as I use it.
Loosely, currents
are the various latitudinal zones possessing different mean rotation
rates.
More precisely, a current is a particular rotation neriod or
velocity which, for many years, is characteristic of a large fraction of
soots in a particular latitudinal zone.
Thus a current is not defined so
much by the belt it is in, or even its latitude, as by its characteristic
rate.
It
often happens that spots in closely adjacent latitudes (or even
the same latitude) follow the notions of two distinct currents.
It also
happens that spots in a particular belt may follow the rate of one current
during some years and another current during others.
more stable in latitude than Some belts.
Some currents seem
Reese and Smith (1966) have
shown that the rapidly-rotating spots in north temperate latitudes (about
240 N.) are manifested on periodic occasions when the Notth Temperate Belt
(ITB)
shifts southward into that latitude.
evidence that the S. S
On the other hand, there is
Temperate Current extended its influence equator-
ward around 1940 when spots on the sough edge of the STB, which had been
rotating about 15 seconds faster at a period corres7onding to that of the
S.
S. Temperate Current.
The mean rotation period of a current can differ
by several seconds from year to year; these are real changes, not statistical fluctuations.
Some currents, such as the S. S.
are more stable from year to year than others.
Temperate Current
For most currents the
rates are often similar from year to year followed by rapid acceleratiQns
or decelerations which mark the start of a new regime which may last for
'''
;=-
" -
I, *
several more years before a returt
to normali
Most currents have fairly sharp latitudinal boundaries, and the
characteristic rotation periods usually differ by substantially greater
amounts than the typical variations from year to year or the deviations
from the mean of different spots within a current.
That is, "currents s
seem to be fairly well-defined entities and are not just arbitrary subdivisions of a smoothly varying latitudinal dependence of wind velocity.
The average rotation periods for individual snots generally differ by only a few seconds from the mean for the current it is in.
Some-
times there are temporary groups of spots, separated from each other by
longitude around the same latitude circle, which move either somewhat
faster or slower than the mean for a current.
Apart from the rotation periods for a current as a whole, or its
longitudinal sections, individual spots have their own characteristic behavior.
Published and un-published drift charts for the N. Ec. Current
suggest that most North Equatorial spots undergo relatively rapid oscillations about their mean longitudinal drift; though non-periodic, the oscillations result in shifts of as much as 100 in a single month.
The
present analysis of photographs shows that this behavior is specially peculiar to the N. Eq. Current.
Published drift charts also indicate occa-
sions when spots suddenly accelerate or decelerate and adopt a lasting new
mean rotation period which may differ by many seconds from the previous
period.
Such changes can occur either as part of a change in a whole
current' or section, or can be quite individual.
Such rapid and unpredict-
able changes in motion make it difficult to trace and identify spots
through even short gaps in observations.
*.4o~
19
As discussed earlier in this section,
these finer aspects of
spot motions have never been systematically studied from either amateur
observations or from photographs, even though suggestions of typical behavior can be seen on the crude drift charts based on CM transits.
The
important point of this section is that while there is regularity and uniformity in the characteristics of Jupiter's circulation over the past
century, or longer, it is also true that many of the characteristics show
temporal variations.
Therefore, the results of the present analysis must
be taken as representative of Jupiter's circulation only during the period under study.
Certainly some gross characteristics derived for one year
will exemplify Jupiter's behavior at all times.
At least some of the fin-
er.aspects of the statistics may be expected to be approximately typical
for a given current, but likely not to within the measured statistical error since other characteristics of currents are known to vary from year to
year.
Certainly
the value of the present investigation will be enhanced if
it is repeated for other apparitions so that the nature and magnitude of
year-to-year changes in the statistics can be ascertained.
A final word of caution is necessary before describing the project.
This is simply an empirical study, with no presumptibn to attempt a
physical explanation at this time, and it
should be emphasized that we are
uncertain yet as to just what we are measuring the motions of when we 'observe "spots N .
It would be naive to assume that the "spots" are dynam-
ically neutral "wind markers".
Spectroscopic observations suggest that
the true rotational velocity of Jupiter's atmosphere above the cloud surface approximates the velocities obtained from spots, but the precision is
poor.
Motions of terrestrial cyclones and anti-cyclones, which may be the
analogues of Jupiter's spots, have been shown to duplicate in relative
20
directions but not in absolute iagnitudes soe of the true dynamical elements of the terrestrial circulation (Macdonald, 1967).
III.
TIE METHODS USED FOR OBTAINING DATA O
JUPITER'S SPOTS
FROM THE PHOTORAPHIC PATROL
A. Construction of Photographic Drift Charts
The early phases of planning the construction of the charts
which were eventually used as the basis for the nresent investigation,
although carried out mainly by myself shall not be construed to be strictly part of the work on this thesis, since much of it was done prior to my
enrollment in M. I. T.
Nevertheless, since these charts form the basic
source for the data used in the thesis, it is necessary to discuss their
format and preparation in some detail for background purposes.
This is
the first such description of'the preparation of the charts.
The Patrol Photographs
The original source of the photographs is the plate collection
at the New Mexico State University Observatory on the campus in Las Cruces,
New Mexico.
The plate collection covers the period of the current decade,
but until about 1964 the coverage was less complete and the photographic
quality not as high as in later years.
21
Prior to February 1967, a 12-inch
aperture reflector, located on Tortugas V1ountain, was used for the patrol
photography.
Since the,
a 24-inch Boller and Chivens Cassegrain instruTwo
ment has been installed on Tortugas Mountain as the patrol telescope.
photographers work on alternate nights to obtain patrol photographs of Venus, Mars, and Jupiter, and more irregular photographs of the other planets.
Photographs are regularly taken with filter-plate combinations sensitive
to red, green, and blue wavelengths.
Occasional photographs are also taken
on ultraviolet or infrared sensitve plates and on panchromatic plates.
The New Mexico photographic patrol of Jupiter is not continuous;
there are the many gaps necessary because Jupiter is too near the sun, or
below the horizon, or behind a cloud, or a particular Jovian loQngitude is
not facing the earth. Also, because of the extreme rarity of perceivable
changes in Jupiter's surface features during the course of rotation across
the disk, it is only necessary to photograph Jupiter once every 2 hours,
or so, to insure complete coverage as the planet rotates beneath us.
But
mainly in the interests of economy, the New Mexico patrol is somewhat less
complete than ideal.
Coverage is often omitted in order to photograph the
other planets, cr because the seeing conditions are rather poor, or because good coverage was acheived just the night before, or for a host of
other reasons.
There is a general attempt to cover a particular Jovian
longitude at least twice a week.
On the average, the coverage is this
good or better during the middle months of. an apparition. Sometimes an
extra effort is made-to photograph particular surface features which
yields superior coverage for certain longitudes compared with
others.
The various scheduling procedures plus urpredictable circum-
22
stances such as cloudy weather occasionally result in gaps in the coverage
in one of the regular colors near a particular longitude of up to a month
even in the middle of an apparition.
There are also cases of nearly daily
coverage of a particular longitude fdr a week or two.
The patrol photographs are not at all of equal quality.
The res-
olution in the images is a function of many factors of which the most important is the "seeing" condition -- small-scale turbulence in the terrestrial atmosphere which either causes "excursion" of Jupiter's image across
The
the plate during an exposure, or simply makes the whole image fuzzy.
seeing varies from second to second; thus many individual exposures must
be made to obtain good images even though, as at the N.M.S.U. Observtory,
the photographer is monitoring the seeing visually at the same time. A
typical N.M.S.U. plate has several dozen images taken during the ccurse of
several minutes.
(The time of each image is accurately recorded.)
The
average seeing also varies from day to day with changing weather and over
the course of an apparition (early and late in an apparition Jupiter must
be observed when low in the sky where seeing is bad).
All N.M.S.U. plates
are examined and the better images on each are marked.
Also a rating of
the average quality of the better images is made on an A,B,0 7 D,E scale;
these ratings are found to correlate closely with the photographers' estimates of the seeing conditions recorded during the observation period.
The Photographic Prints
I decided that the best way to order the New "exico data was to
construct "drift charts" analogous to those used for the analysis of CM
transits, except to substitute photographic strips -- which convey full
information on not only spot longitudes but also their sizes, shapes,
brightnesses,
relative latitudes, etc.
--
in
place of the simple symbols
used to represent CM transit longitude determinations.
By constructing a
separate chart for each latitudinal zone, and laying photographic strips
horizontally on the chart, with left-right position determined by the longitude of the central meridian,
creasing date, it
is
and nesting them beneath each other with in-
possible to follow ct a glance the development and ev-
olution of an entire zone during the period covered by the chart.
This
technique, while less sophisticated than the very difficult task of constructing time-lapse movies from the plates, and somewhat less precise and
objective than machine measurement and interpretation of the plates,
is
well-suited for a relatively rapid, inexpensive pilot project with the aim
of establishing the general characteristics of Jupiter's evolution during
an apparition.
I decided to construct nine charts covering Jupiter's entire
surface with nine slightly overlapping zones.
Since maximum coverage was
desirable not only for the size-lifetime study but also for other general
studies of Juniter such as those described in this thesis, all available
non-redundant plates wer6 used during the year best covered by high quality plates.
Examination of several years of patrol plates suggested that
the time coverage during the latest complete apparition (1966-1987) was at
least as good for previous apparitions,
and the quality of the plates was
somewhat better, mainly due to the installation of the larger telescope
in the middle of the apnarition.
The period selected included the entire
1986-1967 apparition plus the tail
end of the previous annpparition and the
early beginnings of the 1967-1968 apparition (19 months including the two
long gaps near solar conjunctions).
The charts on which the present study
is based cover only the final three-quarters of the 1966-7 apparition and
S:24
11
,. - ~I
~t'r, ,
qt-,
.~-
-.
including one long gap);
the beginning of the next appatiti6n (one j48,
charts for the earlier photographs, many of relatively poor quality, are
not yet completed.
Photographs of Jupiter in different colors show substantially
different surface features.
In order to avoid the confusion of mixing
photographs of different wavelength sensitivity,
separate charts were made
for long-wavelength photographs (red and near infrared) and for short-wavelength photographs (blue and near ultraviolet).
Since green plates show
features intermediate in appearance between red and blue, redundancy was
reduced by omitting any charts based on green photographs, but using green
photographs, when appropriate, to fill in lengthygaps in coverage on both
the blue and red charts.
All the blue and red plates were used except
those for which the quality rating was D or less and except for those which
provided only redundant coverage of a particular longitude already covered
by adjacent photographs taken the same night.
Even poor quality plates
were used when required to fill a gap in the coverage.
The-best images were selected from the chosen plates and used
for making positive prints on flat-lying semi-matte Cronapaque paper.
ing the known plate scales,
the ephemeris for the true angular diameter of
Jupiter from date to date (A.E.N.A.),
ifcation of the enlarger in
and a new calibration of the magni-
the N.M.S.U.
Observatory darkroom,
sible to print all the photographs to the same scale -ter's polar diameter.
successfu
Us-
it
was pos-
5.45 cm to Jupi-
A small exposure meter was used in a not-always-
attempt to produce prints of uniform average brightness.
By projecting the image onto the paper through a snecial photo-
graphic plate overlay, it was -ossible to superimpose on all prints an
accurate outline of Jupiter and other identifying marks used later in
preparation of the charts.
A fine white line was superimposed on all
prints bisecting the Jupiter outline to serve as a marker of the central
meridian for pasting photographic strips at the proper longitudes on the
charts.
Also superimposed on the prints were the meridians for +350 from
the C,.
Because surface spots on Jupiter lose their contrast away from the
center of the disk, I decided to use only the central 700 for placement on
the charts; hence the +350 meridians indicated where the ends of the strips
were to be cut off.
Foreshortening results in a maximum displacement at
the edges of the strips 2?2 in longitude --
sufficiently small to be easi-
ly taken into account in analysing the charts.
prirr,
Also superimposed on each
exterior to the image of the planet itself, were series of marks
indicating the edges of the nine chosen latitudinal zones to serve as
guides for the print-trimmer.
Since the nine zones are slightly overlap-
ping, two identical prints were made of each photograph for staggered cutting.
A nrint of the plate overlay was placed in the movable paperholder so that Jupiter's image could be centered correctly before inserting the unexposed paper and lowering the plate overlay (fastened to the
paper holder).
Because of the non-symmetrical brightness distribution
across the image of Jupiter, except near opposition,
caused by the sun-
Jupiter-earth phase angle, some bias is necessarily introduced in centering the image (phase exaggeration).
correcting for phase exaggeration,
Mr.
Elmer Reese,
who is
familiar with
helped to guide the darkroom assistant
to make appropriate though subjective corrections for phase exaggeration,
but long-term systematic bias of perhaps two degrees is
26
undoubtedly still
present.
gree.
Random error in centering probably amounts to less than one de-
The orientation of the centered image of Jupiter was relatively easy
to accomplish because of the planet's nrominent belts parallel to the equator; in any case the precise orientation is not crucial.
To minimize the effect of the discontinuity in longitude at the
left and right ends of the charts (00 and 360), all images with central
°
meridi-ans within about 250 of either 0 or 360
were'printed twice (4
prints) so that they could be pasted at both ends of the charts.
The Charts
Approximately 700 separate images of Jupiter were used to construct 18 charts which depict the evolution of Jupiter's surface features
in
two colors (red and blue) for the nine different latitudinal regions.
The charts currently cover the 1966-7 apparition from November 2 through
its
conclusion (last photograph June 14) plus the very beginnings of the
1967-8 apparition during the period Sept. 30-November 14.
sents the relevant information about the charts.
Table 1 pre-
The central latitude is
the zenographic latitude , apnroximately in the center of the latitudinal
in
region covered by each chart, for which the longitude scale was chosen
positioning the photographs.
Clearly, because of the different lengths of
latitude circles, the adopted longitude scale on each chart is slightly too
expanded for spots poleward of that latitude.
latitude in
The choice of this central
each zone was weighted toward the latitude where spots were
Actually the latitude assumes that Jupiter's axis is exactly perpendicular
to our line of sight. In fact, Jupiter's north pole was tilted towards'
earth during this period by a varying amount of somewhat less than 1 .
27
most prevalent.
The next column lists the abbreviations of the important
belts and zones covered by each chart.
The penultimate column lists the
ratio in length of lo in longitude at the central latitude to 10 at the
equator; this is useful because later analyses record spot lengths in degrees 'rather than absolute lengths.
Note that the longitudinal scale on
the charts is such that 10 at the equator = 0.20 inch.
The vertical daily
spacing of the photographic strips is given in the last column in inches.
Because of this Yide spacing necessitated by the width of the strips, between 2 and 3 pieces of cardboard 30 inches long were required to cover
the 225 last days of the 1968-7 apparition for each chart.
The photographic prints were sliced into strips with a printtrimmer.
The foreshortened ends of the strins were cut off with scissors,
and the resulting parts rubber-cemented onto the white cardboard charts
In
positioned with the aid of accurate longitude rules for each chart.
cases where two strips overlapped, some effort was made to place the better one on top.
The resulting charts are a montage of strips which when
viewed from a distance seem to show little
and quite random spacing.
uniformity in
tone, few spots,
AltYhough it was not planned that the charts
would ever be striking pictorial exhibits of Jupiter to the untrained eye,
the variable darkness of the strips is
disconcerting and makes any attempt
to copy the charts for illustration in this thesis quite impossible.
The
variable brightness of the strips is due partly to uneven darkroom proce-dures, partly due to poor quality control by the photographic paper manufacturer,
and partly due to the innate variability in
the plate images
affected by observing conditions, plate characteristics- etc.
To the ob-
servant eye, however, these non-uniformities are relatively unimportant,
and hundreds of saots can be discerned and traced from day to day.
Of
more concern are the gaps in coverage, caused either by poor photographic
quality usually caused by poor seeing conditions, or else by a complete
lack of photographs of a particular longitude during a lengthy interval.
The proper sorting out of the real characteristics of the Jovian spots
from the bias due to such coverage problems is a difficult taskc.
The fol-
lowing sections describe my preliminary attempt to obtain this information.
TABLE I
Chart
Central
Latitude
I
430
II
27j
III
18
IV
5X
Ratio 10 Long
at Central Lat. Daily Spato 1 at Eqat. cing (in.)
Belts and Zones
Covered
0.758
0.0350
0.899
0.0300
NTBs, NTrZ, NEEn, NEBZ
0.957
0.0300
NEBZ, NEBs, EZn, EZs
0.996
0.0417
0.990
0.0300
NNTBs
NPR (south),
I11TB,
11TTBs, NTeZ,
ITB, NTrZn
V
-9
VI
-17-
SEBn, SEBZ, SEBs
0.961
0.0300
VII
-24
SEBs, STrZ, STB
0.929
0.0300
VIII
-34,
STB, STeZ, SSTBn
0.851
0.0350
IX
-481
SSTB, SSTeZ, SPR (north)
0.688
0.0300
B.
EB,
EZs,
SEBn
Reduction of Spot Statistics from the Drift Charts
Tracing Spots on Overlays
Before one can compile statistics on the spots, one must iden-
MRefers to unforeshortened longitudes near the central meridian; 10 at
equator = 0.2 inches on the charts.
tify the spots.
In particular, one must unambiguously trace -the spots
from day to day if one is to obtain any information on spot notions or evolution.
As suggested in Section II B, this is a difficult task.
Fortu-
nately it is comparatively easy to discern continuity of spots from the
numerous characteristics revealed in complete photographs of the spots.
Nearly every current has a variety of large, prominent, relatively long-lived spots whose drifts from day to day are clear.
These
spots serve as markers, and the motions and development of smaller spots
can be traced in relation to the larger ones.
Because of the lucid pre-
sentations of the evolution of a region on the charts, one quickly develops an impression of the qualitative characteristics of the spot appearances, motions, and changes which allows one to form subjective but realistic decisions concerning the reliability of interpreting a pair of spots
observed on different days as the same spot.
As discussed earlier, this
approach is a substantial improvement over earlier drift charts, based on
largely heterogeneous data on spot longitudes only.
Nevertheless, the
present techniques are inferior to what can eventually be acheived by obBut in order to establish meaningful
jective analysis of the patrol data.
criteria to serve as the basis for programming the objective decision-making routine, it is necessary to make a pilot study such as the present one
which provides an approximate basis for choosing realistic criteria.
Pencil lines connecting identical spots were drawn on transparent matte-surface overlays.
First a symbol was recorded on the over-
lays to signify each visible spot.
Subsequently, after careful attention
was paid to all the details visible in the photographs, solid lines were
drawn connecting the obviously-identical spots.
30
Dashed lines were used to
connect spots deemed to be probably identical, and .dotted lines used for
possibly identical spots.
In doubtful cases, of which there were many
(particularly for smaller spots), no lines were drawn.
The process was
then iterated to insure that all spots down to a uniform standard of reliability were marked and that complete and uniform construction of the
drift lines was achieved.
The use of different symbols helped to dis-
tinguish spots of different sizes and colors.
Lines of different colors
were used to plot drifts for spots in adjacent but different latitudes
which frequently have different average drifts.
It was not easy to maintain uniformity and reasonable objectivity when marking spots and then drawing drift lines.
It is easy to see
small, rather vague spots on an otherwise featureless belt when spots of
equal or greater size or contrast can be missed amid the general confusion
of such a belt as the NEB. Also, it is undoubtedly the case that an isolated spot moving with a greatly different velocity from its neighbors
(or rapidly oscillating in velocity or latitude) would be harder to detect than a similar spot moving in a normal fashion.
Also there is the
"zebra problem"; whether to call an assemblage of spots dark spots on a
light bacrkground or bright spots on a dull background.
In many cases
there is no doubt as to whether the spots are mainly dark or light, but
in some regions where the spots are ill-defined (such as the wavy edges
of the SEB),
my preference for seeing primarily dark spots might not be
shared by others.
Measured Information about the Spots
From the innumerable kinds of data which could be measured con-
31
cerning each spot, I selected the following representative characteristics
for the pilot study.
They cover, in approximate form, most of the charac-
teristics which can be obtained from the present charts in a reasonably
short time.
The information for each spot was punched on two computer
cards.
Each spot was given a number, ranging upwards from 1.
Number:
Latitude:
The spots were placed in one of the following 24 latitudes.
There are two numbers corresponding to the south component of the NorthNorth-Temperate Belt; number 22 refers to spots seen on the north edge of
the chart for the NTB, while number 23 refers to spots seen on the south
edge of the chart for the NNTB.
2
17 NEBZ
9 SEBsn
1 SSTeZ
SSTB
3 SSTBn
4 STeZ
5 STB
10
SEBZ
18
NEBn
11
SEBns
19
NTrZ
12
SEBn
20
NTBs
21
NTB
22
NNTBs
13 EZs
14
EB
6 STBn
7 STrZ
8 SEBs
23 NNTBs
24 NTNTeZ
15 EZn
16 NEBs
'
Number of observations:
This is the approximate number of dates on which
the spot was recorded.
Dates observed:
The first and last dates on which the spot was definitely
recorded are given.
once.
These dates are the same if the spot was seen only
The 225 days of photographic coverage were numbered consecutively
from 1 to 225 (1 = November 2, 1966).
32
Reasons why not observed before or after:
There are many reasons why a
spot is not seen before or after certain dates.
Perhaps the spot disap-
peared, or perhaps the coverage was poor, or other reasons.
or combinations of reasons, are listed below.
were recorded -
Nine reasons,
For each spot, two numbers
one giving the reason why the spot was not seen earlier,
one why it was not seen afterwards.
o = The spot definitely was not formed or definitely disappeared.
This
includes the cases when smaller spots either emerged from or merged into
larger spots.
1 = The spot Drobably was not formed or probably disappeared (including
probable merges).
2 = The spot was vague or small and was only marginally observed in any
case.
3 = There were lengthy gaps in the photographic coverage either before or
after the spot was observed rendering identifications uncertain.
4 = There were many nearby similar spots, pebhaps exhibiting rapid relative motions, rendering the identification of the spot ambiguous.
5 = Combination of 2 and 3 above.
The spot was vague and the coverage was
poor.
6 = Combination of 2 and 4 above.
The spot was vague and crowded by sim-
ilar spots.
7 = Combination of 3 and 4 above.
There was poor coverage and the spot
was crowded.
8 = The spot continued to exist but had substantially changed its appearance.
9 = The snot could not be followed because one end of its lifetime extended into the time either before or after the photographic coverage of the
1966-7 apparition.
Dates definitely not extbnts
For those spots which were recorded as either
33
definitely not formed or definitely disappeared, the previous or following
dates are given on which there is definite photographic evidence that the
spot was not extant.
These dates help establish upper limits to spot life-
times.
Positions at thirty-day intervals:
The longitudes of the spots were re-
corded for days numbered 15, 45, 75, 105, 135, 165, and 195 if the spots
were extant on any of those days.
Typical deviation from uniform drift:
Different spots show differing
tendencies to meander about a straight line drift.
For each spot which
lasted at least 30 days, an estimate was made of the typical short-term
deviation of the spot (in degrees) from its mean drift during a 30-day
period.
These are listed in the tabulations in the appendix in the column
labelled "DEVI.
Dates of soecial prominence:
S6me spots are visible for a long time, but
have a period or two of unusual prominence.
The beginning and ending dates
of such periods were recorded when applicable.
Snot description:
In order to approximately identify spots by appearance,
the following classifications were applied%
(1) Light or dark.
medium, or sharp in general outline and distinctiveness.
(2) Fuzzy,
(3) Spot propor-
tionss spot length about 3 times its width or longer, spot about 2 times
its width, spot about as wide as it is long, spot about twice as high as
it is long, ahd'.snot much taller than it is long (length here refers to
longitudinal extent).
Some Jovian surface features are borders and are
not characterized by lengths or proportions -- this was noted in such
cases.
(4) Spot type:
round or oval, festoon, wavy edge or projection
from a belt or zone (either dark or light), angular shaped spots, aworphous
spots, variable shape, preceding border, or following border.
Spot lenthst
The maximum and minimum lengths of spots were recorded in
degrees of longitude.
Snot continuationss
It has already been pointed out that for several rea-
sons, the continuous drifts of spots are interrupted by gaps in the coverage or for other reasons, and that in such cases of doubtful drifts, dashed
lines were drawn on the chart overlays to indicate probable spot continuations and dotted lines to indicate possible continuations.
In addition
there are cases of merging or diverging spots, which themselves are either
definite, probable, or possible.
In all these cases, the continuations
were noted by punching the reference numbers of adjoining spots on the
computer data cards.
In any cases of ambiguous continuations of spots, no
more than one continuation is
Physically related snots:
regarded as "ptobable".
On some occasions, it is clear that several
spots are physically related to each other.
For instance, in the north
edge of the NEB there was a small white spot surrounded by a much larger
dark spot.
ent.
It is possible that such combinations are in no way independ-..
The reference numbers of any closely related spots were punched on
the data cards, though no use of such relationships was made in this preliminary study.
All of the above spot characteristics were recorded for the bluelight photographs of all currents except the North Equatorial Current.
The
spots in the North Equatorial Current, unlike the remainder of the planet,
are much more prominent in red light.
In a subsequent study, the red
light photographs of all belts, plus the relatively featureless bluelight photographs of the Equatorial regions,
if
there are any systematic differences in
tion of color.
will be analysed to determine
spot characteristics as a func.
Partly in order to assure uniformity of the data analysed
in this thesis, and partly because of difficulties in computer storage of
the voluminous data on equatorial spots, discussion of the NEB regions is
omitted from this report.
IV.
A.
COIiPUTER A2IALYSIS OF THE OHARACTERISTICS OF JOVIAN SPOTS AND OURRETTS
Spot Characteristics
The-number of spots observed and the numerous computations necessary to derive all the atatistics desired required the use of a computer.
A Fortran IV IBM 360 program of more than 1000 steps was written de-
signed to execute the following procedures.
Definite, Probable, and Possible Spots
The data cards contain information on spots with definitely observed drifts or else spots which were definitely observed only once.
Probable and possible spots were generated from series of definitely observed spots using the continuation reference numbers and the following
-.
°.
36
conventions. Many of the probable and possible drift lines drawn on the
chart overlays are of a branching nature -- i.e. they indicate either
merges or else ambiguous continuations of which only one may be the correct
one.
One could study all possible combinations and permutations of spots
formed by the probable and possible drifts, but for our purposes this
would be mis-representative.
For instance, in the case of the two promi-
nent merging spots in the NEBn, such a procedure would give lifetimes for
both of upwards of 6 months.
But, since during the last 4 months of this
neriod there was only one spot where there had been two, one clearly had
disappeared and both did not last 6 months
Also, to follow both naths in
cases of ambiguity, clearly would not represent the real situation, whereas
to choose and follow just one path in an ambiguous case at least m
rep-
resent what really happened.
Therefore I have traced probable and possible spot drifts using
the same convention in which rivers are usually named.
At each juncture
of two spot drifts (whether due to ambiguity or real merges), only one is
traced past the juncture and the other is regarded as either having disappeared (or appeared in cases of divergence).
Probable spots are taken
as those singly observed spots and definitely traced spots which are connected by one or more probable drift lines.
definite
Possible spots are those
spots and probable spots which are connected by one or more pos-
sible drift lines.
Some of the statistics compiled below are considered separately
for each possible grouping of the observed spots.
The statistics for def-
inite spots may be regarded as providing the most reliable information on
spot drifts, particularly over short periods of'time.
H!owever, because
of the gaps in
the photographic coverage,
the possible spots probably
give the most realistic, though not most reliable, picture of the lifetimes and evolution of spots.
The bulk of the statistics are computed
for the probable spots only.
The second last column of the spot tabulations in the appendix
(labelled "PART") lists the identification number for any probable or
possible spot of which the tabulated definite or probable spot is a part.
In addition to the data measured directly for each spot, the
following characteristics were computed for, each definite, probable, and
possible spot.
Spot Lifetimes
The observed lifetime of a spot is equal to the last date on
which it was observed minus the first date (arbitrarily set equal to 0.5
Howdver; these are clearly minimum
days for spots observed only once),
From these observed lifetimes and the recorded reasons why the
lifetimes.
spots were not observed before or after these dates (see Sect. III B),
more realistic lifetimes for each spot were computed (when possible) and,
in any case, the lifetimes were considered to be in one of six categories
of reliability.
Estimated true lifetimes
If both ends of a spot lifetime were considered
to have been definitely determined (reasons not recorded both coded 0 as
described earlier), then an estimate of the true lifetime was made by averaging
the observed lifetime and the time difference between the two
dates on which the spot was definitely not extant (the latter dates are
recorded when ends of spot lifetimes were observed).
38
-i:
5
Probable lifetime:
If one end df a spot lifdtie was definitely observed
(0), but the other was only probably observed (1), or the spot changed its
appearance drastically but did not necessarily di'sappear (8), the observed
lifetime was taken as the spot's probable lifetime.
Twice probable half-lifetime:
If one end of a snot life-time was definite-
ly observed (0), but the spot history extended beyond the period covered
by the charts (9), a probable but by no means conclusive estimate of the
lifetime is twice the observed lifetime.
Relatively few snots with life--
times of many years would disappear or form during the short period under
observation.
Most spots disappearing during the observed period probably
had lives comparable to the period, especially since there was not a large
population of spots which survived the entire observed period.
Possible lifetime:
If no definite end of a spot history was observed, but
the observed ends were for reasons 1 (probable disappearance) or 8 (changed
appearance), the observed lifetime was considered a possible estimate of
the lifetime.
Twice rossible half-lifetimes
If one half of the spot history extended
outside the observed period and the other end was either probably observed (1) or due to changed appearance (8), twice the observed lifetime was
considered a possible estimate of the lifetime.
Minimum lifetimes
All other combinations of reasons why spots were not
traced either before or after their observed duration yield no meaningful
information concerning the true lifetime.
If
the spot history spanned the
entire period of obs-rvation (both reasons 9), we can only say that its
39
observed history was a minimum 1iiitime foi the spot -en have been permanent, such as the Red Spot.
the spot could ev-
If the spot was lost due to
gaps in the photographic coverage, ambiguity due 'to crowded adjacent spots
and rapid motions, or any of the other reasons coded 2 through 7,
there is
no reliable information on more than the minimum lifetime of the spot.
Un-
fortunately, most spot lifetimes computed in this study are of this type.
The only solution for clarifying information on the lifetimes of many of
the smaller spots is
to obtain improved photographic resolution and --
more importantly -- coverage.
One and only one kind of lifetime was computed for each spot.
These are listed in the tabulations in the appendix in the order described
here.
Asterisks fill the columns for the lifetimes not applicable to the
spot.
The following column, labeled "WHY" gives the reasons why the spot
could not be followed prior to and after its observed period.
Spot Motions
It is customary to record spot motions in terms of longitudinal
drifts relative to the adopted longitude system in
30 days.
If
the 30-
day drift of a spot is called D, and the adopted longitude system rotates
with a period Po (minutes), then the rotation period of the spot is given
by
P
+
(1)
(D)(P2
15552000
Both the mean 30-day drift, computed between the observed longitudes on the first-and last days on which the spot was seen, and the rotation period are listed for each spot in the tabulations in the appendix.
40
The longitude at opposition, given in the fourth column of the tabulations,
is computed from the mean drift for each spot and is not the true longitude
of the spot on date of opposition (day number 80) when many of the spots
were not even extant.
For those soots lasting long enough to have measured positions
at the ends of the six thirty-day intervals,
computed for each interval.
separate 30-day drifts were
To provide a measure of the long'-term devi-
ation from uniform motion of the longer-lived spots, the average deviation
from the mean of these thirty-day drifts ("30DEV")
was computed for each
spot observed during at least two of the periods.
To provide some infor-
mation on systematic changes in motion,
second,
the mean drifts during the first,
and last third of the observed part of the apparition were com-
puted for each long-lived spot extant during those periods (these are called "DRIFTla,
"DRIFT2",
and aDRIFT3" in
the tabulations).
In order to
trace spots across the gap in coverage caused by solar conjunction, the
projected positions of spots on November 1, 1967, were computed for all
spots lost in June due to the end of coverage (these longitudes are not
tabulated here).
Comparison of these longitudes with the spots observed
in NIovember 1967, when combined with knowledge of typical variations in
snot motions computed here, help to identify some larger spots with some
assurance,
even after a gap of four months.
Spot Lengths
The maximum and minimum lengths measured for each spot yield not
only the mean length for each spot,
but also a crude estimate of the typi-
cal deviation in length for the spot.
Tabulated in the column labelled
"DL/L" is the quantity
DL/L
m
max
m
max
min
(2)
(in)/2
Since the accuracy in measuring the lengths of most spots, particularly the
fuzzy ones, is
no better than a degree or two, the quantity DL/L is not
really representative of physical changes.in sizes of spots less than about
half a dozen degrees in length.
Future investigations of the spots will
take such errors into account quantitatively.
B.
Characteristics of Currents
The mean 30-day drifts for spots in each current were computed
in two ways, neither of which is exactly identical to the procedures used
in reductions of visual
f01transits.
First tabulated is the mean drift for
all spots (except those observed only once), weighted by the number of observations of the spots.
The weighting reduces the scatter caused by the
unreliable drifts of very short-lived snots, but gives perhaps undue weight'
to the prominent and long-lived spots.
More comparable to the mean drifts
calculated by amateur astronomers are unweighted averages of the mean
drifts of all spots with observed lifetimes of 10 days or more.
For both
types of calculation of mean current drifts, the average deviation of the
individual spots from the current mean is also tabulated.
Both weighted and unweighted mean drifts (and average deviations)
were also computed for dark spots,
light spots,
long spots (length over
7T5), and short spots (less than 705) in each current separately.
All of the above compdtations were made separately-for three
groups of spots:
the definite spots, the definite and probable spots, and
the definite-probable-possible spots.
Just the definite-probable sample of spots was used for calculating additional mean characteristics for each current.
following:
These include the
the mean of the long-term deviations of the six 30-day drifts
from the spots' mean drifts; the mean of the typical short-ter
in degrees from the spots' mean drifts
deviations
during 30-day intervals; the mean
drift of all of the longer-lived spots in the current during the first,
second, and last thirds of the apparition; the mean lifetime of those spots
for which either definite or probable lifetimes were computed (the first
four of the six lifetime categories); the mean proportion of spots in the
current; the mean length of spots; and the mean DL/L length-deviation ratio of spots.
Also presented are tables showing the distribution of spots
by type and the size-frequency relationship for spots in each current.
The numbers tabulated in each interval of length are the sums of the observed lifetimes of spots of that size; this yields a good approximation
to the size distribution one might expect to see at any particular instant
in
0.
time.
Relationshins between Spot Characteristics
In order to test for any possible relationship between the size,
shape, motion, color, or lifetimes of spots, all observed spots (without
regard to current) were subdivided according to each characteristic and
the means of the other characteristics were computed.
The mean characteristics which were computed weres
the mean of
the long-term deviations from the individual 30-day drifts; the mean of the
short-term deviations from mean drifts during 30 days; the mean lifetime
for those spots having either probable or.definite lifetimes computed; the
mean proportion; the mean length; the mean ratio of length deviation to
length; the mean signed deviation of spot drifts from the means of the currents of which the spots are part; the number of dark and light spots; and
the distribution of spots by type.
The populations of spots for which the above characteristics
were computed were:
dark spots; light spots; spots less than 50 in length;
spots elongated by a ratio near or exceeding 3; spots longitudinally elongated by a factor of about 2; approximately round spots; spots with latitudinal extents exceeding longitudinal lengths by a factor of about 2; spots
with latitudinal elongations near or over a factor-of 3; spots drifting at
least 30 per 30 days faster than the mean of their currents; spots moving
similar to their currents; and spots moving at least 30 per 30 days slower
than their currents.
D.
Size-Lifetime Relationships
The preliminary numerical results of the size-lifetime relationship under study by R. Hide and the present author (for lifetimes measured
in Months or less), are presented in the final tables in the appendix.
Since it is uncertain whether spot lengths, or their total dimensions may
be the physically most-meaningful parameter, the lifetimes are tabulated
both in relationship to the mean length and to the mean area, where spot
area (in
square degrees) was computed approximately from the crude propor-
tion estimates.
The meaf of each of the six lifetimes is entered for sev-
en sub-divisions by length or area.
ticular category.
Asterisks indicate no spots in a par-
It can be seen from the tables that it is relatively
difficult to obtain reliable lifetimes for the smaller sots and that their
frequently shorter observed lifetimes are really just minimum lifetimes interrupted by gaps in good quality photographic coverage.
V.
SU4~MARY OF COO1CLUSIONS
The empirical approaches described earlier have been applied,
as a start, to all observed spots in the northern hemisphere of Jupiter
(excluding the equatorial jet).
The results, presented in
the appendices,
are largely self-explanatory and require little amplification here.
I
will, however, summarize some of the more obvious conclusions, after
this word of caution:
In assessing the significance of the differences in
characteristics between groups of spots, it is important to take into
account the sizes of the spot data samples being compared.
These numbers
are printed out explicitly only in Appendix 0; however the complete tabulations in Appendix B provide the same information.
The comparisons of the spot populations of the three zonal
regions containing statistically .-
nificagt ntbers of spots, the INEBZ,
INTB, and NEBn, reveal certain important differences.
For instance, while
the drifts of the individual spots in the 1iEBn generally vary from the
mean drift for the current by only a few seconds, there is a substantially
larger deviation in the NEBZ.
This is, perhaps, to be expected since the
NEBZ is the location of the strong latitudinal shear between the equatorial jet and the higher latitudes. Also, for the NEBZ and NTB, both dark
spots and smaller spots seem to rotate more rapidly than light spots and
larger spots.
This may reflect some real variability of motion with
color, but it is also possible that it simply reflects a small-scale
variation in drift velocity with latitude since white spots and dark
spots (for instance) in any given region do not necessarily average to
the precise same latitude,
The size-frequency tables are similar for the three regions in
showing a peak frequency near 5 km.
This may represent a true preferred
size for eddies on Jupiter, but more likcely this simply reflects the
setting in of incompleteness in the tabulations of the less-well-defined
spots smaller than 50 due to resolution limitations of the photographs.
The incremental population index of the spot size distribution is about
-3 in the range 5 to 20 degrees; -3 is a dimensionally significant population index and should be compared with other meteorological scale
distributions.
The mean sizes and mean proportions of the spots are similar in
the three regionsi however, the distributions of spots by type show
significant differences.
The sorting of spots in all latitudes into different groupings,
p
presented in Appendix C,
demons
between spot characteristics.
-i-~
t:Os surp kiiigly
few strong correlations
Among the relationships which do seem
significant are the tendency for dark spots to be rounder in
comparison
to more longitudinally-extended light spots, and the tendency for shorter
spots to be rounder than the more longitudinally elongated longer spots.
This last correlation may be expressed as a tendency for spots to be of
relatively constant latitudinal width despite the longitudinal extension -undoubtedly due to the strong'zonality of Jupiter's atmosphere imposed by
the planet's rapid rotation.
Note also that longer spots tend to vary
in length during their lifetimes more than do the shorter ones.
The results on the lifetimes of spots are, unfortunately,
tively inconclusive in this preliminary reduction of the charts.
size-lifetime tables show little
rela-
The
relationship between those parameters.
Appendix A would seem to suggest that the lifetimes of spots in the NEBZ
(the region of strong shear) are less than in
might expect,
the other regions,
but observational bias renders the fact uncertain.
column labelled "iTY"
in
as one
As the
the spot tabulations indicates, the general
complexity of the NEBZ and the highly variable rates of drift in that
region,
render difficult the reliable determination of lifetimes; these
uncertainties would bias against reliable determinations particularly of
long lifetimes.
Even for the relatively predictable NEBn, about half of
the spots have completely undetermined true lifetimes.
Further considera-
tion of the problems of determining spot lifetimes from the patrol photographs is
in
progress.
Preliminary comparison of the spot tabulations with the reduction
of amateur astronomers'
many disagreements.
data for the same period (Budine,
1968),
reveals
Consideration of the reasons for these disagreements
would be a fruitful direction for further research,
especially since
comprehensive reductions of the photographic patrol plates such as this
one are not being planned on a regular basis and the amateur. reductions
will be the only published information on Jupiter's spots for some years
to come.
VI.
ACOiOWLEDGEMt;
I first wish to thank Prof. Raymond Hide for his guidance and
encouragement in early phases of my work on the Jupiter photographs. His
enthusiasm for the study rekindled my earlier interest as a teenager in
observational studies of Jupiter.
Prof. Victor Starr has been very kind
and concerned in overseeing the thesis to its completion.
I have had use-
ful discussions eith Dr. Norman Gaut and Dr. 'NormanMacdonald.
My wife
Jennalyn did the typing and was quite patient during the hectic last two
weeks.
The preparation of the photographic prints used for constructing
the charts which served as the basis for this thesis was carried out under
sub-contract to M.I.T. by New IMexico State University.
Mr.
:r. Bradford Smith,
Elmer Reese, Mr. Thomas Kirby, and the rest of the staff of the N.M.S.U.
Observatory were very cooperative throughout the project and hospitable
during several lengthy visits I made to New Mexico.
Mr. R. B. Minton was
particularly helpful in solving some practical problems in producing the
prints, most of which were made by Mrs. Judy Solberg.
The construction of the charts, as well as the first part of my
research assistantship, was supported by N.S.F. Grant GP 5053.
The last
terms of my assistantship, and minor additional costs in the analysis were
supported by Contract AF96267-CC9 to the Air Force Cambridge Research
Laboratories.
vII
REFERE!CES
1968, Jupiter in 1966-67: Rotation Periods, Journal of the
Budine, P. W.,
Association of Lunar and Planetary Observers, 21, 13 -- 23.
Chapman, 0. R., 1962, The 1961 A.L.P.O. Simultaneous Observation Program,
Journal of the Association of Lunar and Planetary Observers,
18, 56 -
69.
Chapman, C.
R.,
35,
Telescope,
Chapman,
1968a, The Discovery of Jupiter's Red Spot,
0. R.,
Sk. and
276 - 278.
1968b, Momentum Transfer in Jupiter's Atmosphere, un-
published manuscript.
Hide,
R.
and Chapman,
Macdonald, N.
J.,
C. R.,
1968,
in
preparation.
1967, The Dependence of the Motion of Cyclonic and
Anticyclonic Vortices on their Size, Journal Atmos. Sci., 24, 449452.
1958, The Planet Jupiter (London: Faber and Faber).
Peek, B. M.,
Reese, E. J.,
1961-62,
1982,
Rotation Periods on Japiter During the Apparition of
Journal of the Association of Lunar and Planetary Observers,
18, 193 - 205.
Reese, E. J.
and Smith, B.
A.,
1966,
North Temperate Belt, Icarus, 5,
A Rapidly Moving Spot on Jupiter's
248 - 257.
VIZI.
APPE1DICES
These appendices contain tables printed out by the computer and
comprise the quantitative results of the present study.
The tables are
not numbered but come in 4 parts.
(A.)
The first appendix lists the characteristics of the spot
populations in each of the currents studied.
The tabulations are self-
explanatory and are described in Section IV-B.
(B.)
The second appendix comprises the tabulations, by current,
of all the individual spots measured or generated as probable or possible
conglomerates.
ence number; (2)
The columns are as follows.
First page:
(1) Spot refer-
Limiting day numbers on which spot was observed (Nov.2,
1966 = day 1); (3) Projected longitude on date of opposition (day 80); (4)
Number of observations of the snot; (5)
Mean 30-day drift (degrees); (6)
Rotation period; (7) Dark = 1, light = 2; (8) Fuzzy = 1, medium = 2, sharp
= 3; (9) Spot proportions, 1 = long, 3 = round, 5 = tall,
Spot type:
0 = round or oval, I = festoon,
0 = border; (10)
2 = wave or projection,
3 =
angular, 4 = amorphous, 5 = variable shape, 6 - preceding border, 7 = following border; (11) Length in degrees; (12) Ratic
of deviation in length
to length; (13) Short-term deviation in driPt (degrees).
Second page:
(1)
Spot reference number; (2-4) 30-day drifts during 1sts 2nd, and last thirds
of period; (5)
Mean deviation of succesive 30-day drifts; (6) Lifetimes;
(7) Reasons why spot not followed before or after observed period (see
Sect. III-B); (8) Days when particularly prominent.
(C.)
The third appendix lists the mean characteristics of 12
sub-divisions of all the spots.
These tabulations are also self-explan-
atory.
(D.)
The last appendix is short and is a tabulation of the life-
time-length and lifetirme-area relationship, as described in Sect. IV-D.
Note:
In these appendices,
asterisks are used in place of blanks.
These
usually indicate that there were no computed numbers in the particular
category, usually because of no data.
Several cases probably exist where
numbers are omitted because of computational errors; the computer was
programmed to store numbers larger than permissible by the output format
for a variety of situations in which input data inconsistent with the
logical flow of the program would otherwise have yielded incorrect re-
sults.
52
c
APP-EDIX A
Characteristics of Currents
Note:
As can be seen from the spot tabulations in Appendix B,
three currents (NEBZ,
only
NEBn, NTB) have a sufficiently large population
of spots to permit meaningful intercomparisons of the mean characteristics
given in Appendix A.
THE
FOR
MEAN
ME4N
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
NEBZ
OEFINITE SPOTS
30-DAY DRIFT, ALL SPOTS, WFIGHTED BY NO. OF OBSERVATIONS =
-31.1
AV. DEV= 22.22
-19.0
AV. OEV=
9.26
DRIFT, ALL SPOTS (OpSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
DRIFT,
-30.1
AV. DEV= 19.21
DRIFT, LIGHT SPOTS (OVER 10 DAYS), UNNEIGHTED =
5.06
AV. DEV=
-14.8
=
-20.8
DRIFT, SMALL SPOTS (UNWEIGHTED)
AV. DEV= 11.85
-12.0
AV. DEV=
5.58
=
DRIFT,. LARGE SPOTS (UNWEIGHTED)
DRIFT, DARK SPOTS (WEIGHTED)=
-37.4
AV. DEV= 21.28
DRIFT, LIGHT SPOTS (WEIGHTED)
=
-29.4
AV. DEV= 22.00
=
-34.9
AV. DEV = 25.93
DRIFT, SMALL SPOTS (WEIGHTED)
DRIFT, LARGE SPOTS (WFIGHTED)
=
-21.2
AV. DEV=
9.08
FOR DEFINITE
' F AN
MEAN
MEAN
M EAN
iE AN
MEAN
MEAN
MEAN
MEAN
MEAN
30-DAY
DR IFT,
DRIFT,
DR IFT,
DRTFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
30-DAY
DR IFT,
DRIFT,
DRIFT,
CR IFT,
DRTFT,
DRIFT,
DRIFT,
DRIFT,
CRIFT,
AND PROBABLE
SPOTS
-32.1
AV.
DEV= 22.37
DRIFT, ALL SPOTS, WEIGHTED BY Nn. OF OBSERVATIONS =
A V. DEV= 16.38
ALL SPOTS (ORSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
-26.7
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
-44.6
AV. D EV= 30.22 ,
3.30
LIGHT SPOTS (OVER 10 DAYS),
UNWEIGHTED =
-16.7
AV . DEV=
SMALL SPOTS (UNWEIGHTED) =
-21.4
AV. DEV= 10.25
LARGE SPOTS (UNWFIGHTED)
=
-14.7
AV. DEV=
2.88
DARK SPOTS (WEIGHTED)=
-42.3
AV.
DEV= 73.70
LIGHT SPOTS (WEIGHTED) =
-29.0
AV. DEV= 20.87
SMALL SPOTS (WEIGHTED)
=
-33.6
AV. DEV= 73.92
-21.5
AV. DEV=
9.02
LARGE SPOTS (WEIGHTED)
=
FOR DEFINITE,
MEAN
MEAN
MEAN
MEAN
MFAN
MFAN
MEAN
MEAN
MEAN
MEAN
CURRENT
PROBABLE,
AND
POSSIBLE
SPOTS
-32.9
AV. DEV= 23.19
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
AV. DEV= 19.79
-30.4
ALL SPOTS (ORSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
DARK SPOTS (OVER 10 DAYS), UNWFIGHTED
-47.4
AV. D EV= 28.02
9.34
-21.2
AV . DEV=
UNWEIGHTED =
LIGHT SPOTS (OVER 10 DAYS),
SMALL SPOTS (UNWEIGHTED)
=
-74.8
AV. DEV= 13.83
LARGE SPOTS (UNWFIGHTED)
=
-31.1
AV. DFV= 21.79
DARK SPOTS (WEIGHTED)=
-44.7
AV. DEV= 24.62
AV. DEV= 20.85
=
-29.2
LIGHT SPOTS UWFIGHTED)
SMALL SPOTS (WEIGHTFD)
=
-34.2
AV.
DEV= 24.73
LARGE SPOTS (WEIGHTED)
a
-23.5
AV. DEV= 12.07
THE NEBZ
FOR DEFINITE
MEAN
MEAN
MEAN
MEAN
ME AN
MEAN
MEAN
MEAN
MF AN
CURRENT
AND PROBABLE
SPOTS
CF LONG-TERM DEVIATIONS FROM SPOTS'
MEAN DRIFTS=
1.50
OF TYPICAL SHORT-TERM DEVIATIONS (DFG.)
FROM SPOTS' MEAN POSITIONS=
*****
DRIFT, ALL SPOTS,
FIRST 3RD OF APPARITION=
-14.4
CRIFT, ALL SPOTS, SECONC 3RD OF APPARITION=
******
DRIFT, ALL SPOTS, LAST 3RD OF APPARITION=
******
LIFETIMF (DAYS), ALL SPOTS WITH DEFINITE CR PROBABLE LIFETIMES COMPUTED=
34.5
PROPORTION, ALL SPOTS=
,.3
LENGTH OF ALL SPnTS=
5.6
RATIO OF TYPICAL DEVIATIONS IN LENGTH TO LENGTH, ALL SPOTS, (WEIGHTED)=
0.26
DISTRIRUTION OF
0- 1
0.0
1- 2
0.5
2- 3
17.5
N4 X LIFE-
10-11
0.0
11-12
0.5
12-13
104.0
LENGTH=
N X LIFE=
20-21
0.0
21-22
0.0
22-23
0.0
EFNGTH=
N X LIFE=
L ENGT -=
3-
SPOTS BY LENGTH
4
4- 5
49.0
5- 6
199.0
6- 7
94.5
7- 8
1.0
8- 9
0.5
9-10
45.0
13-14
0.0
14-15
0.0
15-16
0.0
16-17
0.0
17-18
0.0
18-19
0.0
19-20
0.0
23-24
0.0
74-25
0.0
25-26
0.0
26-27
0.0
27-28
0.0
28-29
0.0
29-**
0.0
30.5
DISTRIBUTION
TYPE
NUMBER
OVAL
28
SLANT FESTOON
0
WAVE
2
(DEGREES)
OF SPOTS BY
ANGULAR
1
TYPE
AMORPHOUS
14
VARIABLE
2
PREC. END
7
FOL.
7
END
THE NEBN
CURRENT
FOR DEFINITE
SPOTS
MEAN 30-DAY DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
2.69
DEV=
AV.
-13.1
MEAN DRIFT, ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE),
UNWEIGHTED =
3.49
-12.3
AV. DEV=
MFAN ORIFT,
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
-11.6
AV. DEV=
3.79
MEAN DRIFT, LIGHT SPOTS (OVER 10 DAYS),
3
UNNEIGHTED =
-12.9
AV. DEV=
MEAN DR IFT, SMALL SPOTS (UNWEIGHTED)
=
-12.7
AV. DEV=
3.36
MEAN DRIFT, .LARGE SPOTS (UNWEIGHTED)
=
-12.4
AV. DEV=
3.08
MEAN DRIFT, DARK SPOTS (WEIGHTED)=
-12.6
AV. DEV=
2.69
MEAN DRIFT, LIGHT SPOTS (WEIGHTED)
=
-13.3
AV. DEV=
2.72
MEAN DRTFT, SMALL SPOTS (WEIGHTED) =
-13.1
AV.
DEV=
2.95
MEAN DR TFT, LARGE SPOTS (WFIGHTED)
=
-13.3
AV. DEV=
1.83
FOR
.
MEAN
MEAN
-::
MEAN
-MEAN
t4AN
MEAN
MEAN
MEAN
MEAN
MEAN
30-DAY
DRIFT,,
DRIFT,
ORIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DEFINITE AND
30-DAY
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
CRIFT,
DRIFT,
DRTIFT,
DRIFT,
SPOTS
DEV=
2.47
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
-13.1
AV,
3.27
A V. DEV=
ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
-12.5
3.79
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
-11.6
AV. DEV=
-13.1
AV . DEV=
3.01
UNWEIGHTED =
LIGHT SPOTS (OVER 10 DAYS),
SMALL SPOTS (UNWEIGHTED)
=
-12.8
AV. DEV=
2.97
LARGE SPOTS (UNWEIGHTED)
=
-12.6
AV.
DEV=
3.27DARK SPOTS (WEIGHTED)=
-12.6
AV. DEV=
2.69
=
-13.3
AV. DEV=
2.35.
LIGHT SPOTS (WEIGHTED)
SMALL SPOTS (WEIGHTED)
=
-13.0
AV. DEV=
2.53
LARGE SPOTS (WEIGHTED)
=
-13.8
AV. DEV=
1.98
FOR DEFINITE,
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
PROBABLE
PRORBALE,
AND POSSIBLE SPOTS
DRIFT, ALL SPOTS, WEIGHTED BY NO. nF OBSERVATIONS =
-13.1
AV. DEV=
2.47
ALL SPOTS (ORSVD LIVES 10 DAYS )ORMORE), UNWEIGHTED =
-12.5
AV. DEV=
3.27
DARK SPOTS (OVFR 10 DAYS), UNWEIGHTED
-11.6
AV-. DEV=
3.79
-13.1
AV. DEV= 3.01
LIGHT SPOTS (OVER 10 D)AYS),
UNWEIGHTED =
SMALL SPOTS (UNWEIGIITED)
=
-12.8
AV. DEV=
2.97
LARGE SPOTS (UNWEIGHTED)
=
-12.6
AV. DEV=
3.27
DARK SPOTS (WEIGHTED)=
-12.6
AV.
DEV=
2.69
LIGHT SPOTS (WEIGHTED) =
-13.3
AV. DEV=
2.35
SMALL SPOTS (WEIGHTED)
=
-13.0
AV. DEV=
2.53
DEV=
1.98
=
-13.8.
AV.
LARGE SPOTS (WEIGHTFD)
THE NEBN
FOR DEFINITE
M EAN
MEAN
MEAN
MEAN
MEAN
MEAN
ME AN
MEAN
MEAN
CURRENT
AND PROBABLE SPOTS
OF LONG-TERM DEVIATIONS FROM SPOTS' MEAN DRIFTS=
1.97
OF TYPICAL SHORT-TERM DEVIATIONS (DEG.) FROM SPOTS' MEAN POSITIONS=
2.00
-14.2
DRIFT, ALL SPOTS, FIRST 3RD OF APPARITION=
-13.8
DRIFT, ALL SPOTS, SFCOND 3RD OF APPARITION=
******
DRIFT, ALL SPOTS, LAST 3RD OF APPARITION=
LIFETI.ME (DAYS), ALL SPOTS WITH DEFINITE OR PROBABLE LIFETIMES COMPUTED=
123.4
PROPORTION, ALL SPCTS=
2.4
5.1
LENGTH OF ALL SPOTS=
RATIO OF TYPICAL DEVIATIONS IN LENGTH TO LENGTH, ALL SPOTS, (WEIGHTED)=
0.28
DISTRIBUTION
LENGTH=
N X LIFE=
0- 1
0.0O
,OF SPOTS BY LENGTH (DEGREES)
1- 2
0.5
2-- 3
137.0
3- 4
644.5
4- 5
435.0
5- 6
207.0
6- 7
432.0
7- 8
268.0
8- 9
36.0
9-10
41.0
LENGTH=
-if X LIFE=
10-11
99.0
11-12
133.0
12-13
0.0
13-14
0.0
14-15
15-16
0.0
0.0
16-17
0.0
17-18
0.0
18-19
0.0
19-20
0.0
LENGTH=
N X LIFE=
20-21
0.0
21-22
0.0
22-23
0.0
23-74
0.0
24-25
0.0
25-26
0.0
26-27
0.0
27-28
0.0
28-29
0.0
29-**
DISTRIBUTION
TYPF
NUMBER
OVAL
21
SLANT FESTOON
0
WAVE
?
OF
ANGULAR
1
SPOTS
0.0
BY TYPE
AMORPHOUS
11
VARIABLE
0
PREC. END
7
FOL.
7
END
L911
- 971
NV9 W
'J.31bc
( 03J.N'J3M) S.LUdS 35dVI
LlIi 0*0
=A3f *A
=(C0dIH9IJM) SlUdS 11VWS
0O0 =A30G *1AV
osNV -3W
':13
SI0dS 1W~)11
8 *Zt=((llLLH )IAM)
9,1
=A36 *AV
*****
=A30 OA
******';
=(01W)1HUM)
SIl~dS >IbVC
(031H91 3MN(i ) SIA~hS 398VI 'iJI~i0 NVW
u11 L
U0*0
=A30 "AV
0*0 =A30 *AV
0* sI =(031HUI13MNl) SI.OdS
11WS
1JI
i NV1W
E2c1031H9)13M~Nl ' (SAVU 01 b3AU) SiOdS 1H91
L91
=A30 *AV
4.1=1
bGNV3WA
3***
1W))1iMNf
1
' (SAVO 01 b9AU) Sil~cS )4biG
*****c
=A30 *AV
JLUSAVGi 01 S-3A11 UAL)) Sl~dS hI'V
3LH513MNn 'C3AiOk
AVG-QZ NV3W
4S1IcS 11V *LIilG
=SN011VAVi3Sb0 =W 'ON AO 33J.Hith1
i *E=A30 *AV
=A3G *AV
gazl-
=
S.L0dS 3111ISS~d OJNV
'91T3VUUd 631INIIJ30 bJ
SI0dS 39bIl 4 J31bU Nv~wJ
= (31iHOIJ3M)
Loll=A30 *AV
000
= (03Lfr tI1M1 S.L~dS 11VWS
0'YE-)1
0*0
=A30 *AV
'J1cJb NV3hW
=(03ELWOi3M) S10dS 1LH011 '.I '0 NVDh4
W~zl=A30 'AV
84''l
='**(G
A IIHO)1BM) S.LUdS N4dVG
***=A30 ."AV
L*tl=
((hLH!9IMNn) Si~dS 39bVI
=A30 *AV
000
0'aV(UEIIHOL3I'iNM SIUdS 11WS
=A30 *AV
000
41=1180
NV3W4
UEI1,HIDMNn '(SAVO 01 b AO) SI~dS IH91I
f£'C=A30 *AVL901
1:J -d' NV 3W
031I13IMNAl '(SAVO 01 ~bAU) SiOd-S )116VU
******
*****
='A90 *A
SAVO 01 S31AV I ASU0) SlUdS YIV
031HO)IRMNn '(Bbow b
=A30 *AV
'EEl
L91
J0 *ONAd CEIHtJ13M 'SI~dS 11V 61JJdG
=SNQUIiVAdA3SU1I
9,zlA30 OAV
8,1 I
SLUdS 311V]00Jd ONV -.lINLJ3
b0J
= (0311Il Si.0dS 3 )dVl
eli1=A30G *AV
0'0
=(03iW1I M) Si~dS l1VWS
1*"120*0 =A30 *AV
=
(C.131IJM) SLOdS iHD I
AV
i£'"II=A-30U
LV* i
***=A3U 'A
(0c'**
UiH )I:M) SIUdS >IdV
(031HO91Mnf) SAdS 30bV1
=ABU *AV
L 011 0'U
SiOdS flVWS
='**A30 *AV
**'~=(0J31LHI3MNfl)
UiU Jfl '(SAVO 01 13A0) SiUdS ILH9 1L*1= (Il
0*0
=A U *AV
G31H5)IJMNfl '(SAVO 01 i13A0) SI0dS Nb~V0
*****
=A3G OAV
******
OGIH0I3MNO "(3 iGW bO SAVOI 01 S3AIT GASWi0) SiOCIS 11V
Lo1L0*0
=A30 *AV
= SN0IIVA83SI80 =0 *UN AUd GO3.LW1M 'SiL~dS 11V 41Ib~G
E*',1=A30 *AV
LS*E
61:11 bU NV~iW
'-l bd0 NV3W
'11
O NViiW
4i_41 O NVJW
'dl
SO NV3bW
AVG-01
NV3kW
Si0dS 311NI=00 bDJ
lNgbbf13
thIdN 3Nl
THE NTRZ
FOR DEFINITE
MEAN
MEAN
MEAN
MFAN
MEAN
ME AN
MEAN
MEAN
ME-AN
CURRENT
AND PROBABLE
SPOTS
OF LONG-TERM DEVIATIONS FROM SPOTS' MEAN DRIFTS=
***
CF TYPICAL SHORT-TFRM DEVIATIONS (DEG.) FROM SPOTS' MEAN POSITIONS=
*****
******
DRIFT, ALL SPOTS, FIRST 3RD OF APPARITION=
SECOND 3RD OF APPARITION= -*****
DRIFT, ALL SPOTS,
*4* *
DRIFT, ALL SPOTS, LAST 3RD OF APPARITION=
LIFETIME (DAYS),
ALL SPOTS WITH DEFINTTE OR PROBABLE LIFETIMES COMPUTED=.
*****
2.4
ALL SPOTS=
PROPORTION,
LENGTH OF ALL SPOTS=
s.1
RATIO OF TYPICAL DEVIATIONS IN LENGTH TO LENGTH, ALL SPOTS,
(WEIGHTED)=
0.08
DISTRIBUTION
LENGTI-=
SNX LIFE=
0- 1
0.0
OF
SPOTS
BY LENGTH
(DEGREES)
1- 2
1.0
2- 3
0.0
3- 4
0.5
4- 5
0.5
5- 6
14.5
6- 7
0.0
7- 8
0.0
8- 9
0.0
9-10
0.0
LENGTH=
,N X LIFE=
10-11
18.0
11-12
0.0
12-13
0,0
13-14
0.0
14-15
0.0
15-16
0.0
16-17
0.0
17-18
0.0
18-19
0.0
19-20
0.0
LENGTH=i
N X LIFE=
20-21
0.0
21-22
0.0
22-23
0.0
23-24
0.0
24-25
0.0
25-26
0.0
26-27
0.0
27-28
0.0
28-29
0.0
29-**
0.0
DISTRIBUTION
TYPE
NUMBER
OVAL
5
SLANT FESTOON
2
WAVE
4
OF SPOTS BY TYPE
ANGULAR
0
AMORPHOUS
1
VARIABLE
0
PREC.
7
END
FOL.
7
END,
THE
NTBS
CURRENT
FOR DEFINITE SPOTS
MEAN 30-DAY
MEAN DRIFT,
MEAN DRIFT,
MEAN .DRIFT,
ME AN DRIFT,
MEAN DRIFT.,
MEAN DRIFT,
MEAN DRIFT,
MEAN CRIFT,
MEAN DRIFT,
0.0
AV. DEV=
32.7
DRIFT, ALL SPOTS, WEIGHTED BY NOl. OF OBSERVATIONS =
0.0
AV. D.EV=
32.7
UNWEIGHTED =
ALL SPOTS (ORSVD LIVES 10 DAYS OR MORE),
AV. DEV= *****
******
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
0.0
AV. DEV=
32.7
LIGHT SPOTS (OVFR 10 DAYS), UNWEIGHTED =
0.0
AV. DEV=
32.7
=
SMALL SPOTS (UNWEIGHTED)
.***** AV. DEV= ***~*
=
LARGE SPOTS (UNWEIGHTED)
AV. DEV= *****
****)=
DARK SPOTS (WFIGHTED
0.0
DEV=
AV.
32.7
=
LIGHT SPOTS (WEIGHTED)
0.0
AV. DEV=
32.7,
SMALL SPOTS tWEIGHTED) =
DEV= ****
AV.
c*****
LARGE S.POTS (WEIGHTED) =
FOR DEFINITE AND PROBABLE
-A
SPOTS
0..0
AV. DEV=
32.7
ME AN 30-DAY DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
0.0
DEV=
AV.
32.7
=
MEAN DRIFT, ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE), UNWEIGHTED
*****
DEV=
AV.
**,***
ME
AN DRIFT, DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
MEAN
0.0
AV. DEV=
32.7
UINWEIGHTED =
CR IFT, LIGHT SPOTS (OVER 10 DAYS),
0.0
DEV=
AV.
32.7
=
DRIFT, SMALL SPOTS (UNWEIGHTED)
AV. DEV= *****
**~*
=
DRIFT, LARGE SPOTS (UNWEIGHTED)
DFV= *****
AV.
b*'***
MEAN DRIFT, DARK SPOTS (WEIGHTED)=
0.0
AV. OEV=
32.7
DRIFT, LIGHT SPOTS (WEIGHTED) =
MEAN ODRIFT,
0.0
AV. DEV=
37.7
SMALL SPOTS (WEIGHTED) =
MEAN
*****
AV. DEV=
****
MEANI DRIFT, LARGE SPOTS (WEIGHTED) =
FOR DEFINITE,
MEAN
MEAN
MEAN
SMEAN
MEAN
ME AN
AN
'ME
MEAN
ME AN
'MEAN
30-DAY
DR IFT,
DRIFT,
DRIFT,
ORIFT,
DRIFT,
DRIFT,
DRIFT,
CRIFT,
DRIFT,
PROBABLE,
AND
POSSIBLE
SPOTS
AV. DEV=. 0.0
32.7
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
0.0
AV. DEV=
32.7
=
UNWEIGHTED
ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE),
*****
DEV=
AV.
******
UNWEIGHTED
DARK SPOTS (OVER 10 DAYS),
0.0
AV. DEV=
32.7
LIGHT SPOTS (OVER 10 DAYS), UNWEIGHTED =
0.0
DEV=
AV.
32.7
SMALL SPOTS (UNWEIGHTED) =
AV. DEV= *****
*
**
LARGE SPOTS (UNWEIGHTED) =
**m**
DEV=
AV.
***~*
DARK SPOTS (WEIGHTED)=
0.0
DEV=
AV.
32.7
=
LIGHT SPOTS (WEIGHTED)
0.0
DEV=
AV.
32.7
=
SMALL SPOTS (WFIGHTED)
*****
DEV=
AV.
****
=
LARGE SPOTS (WEIGHTED)
___
THE NTBS
FOR DEFINITE
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MFAN
MEAN
MEAN
AND
PROBABLE
SPOTS
*****
OF LONG-TERM DEVIATIONS FROM SPOTS' MEAN DRIFTS=
*****
FROM SPOTS'
MEAN POSITIONS=
CF TYPICAL SHORT-TERM DEVIATIONS (DFG.)
*****
DRIFT, ALL SPOTS, FIRST 3RC OF APPARITION=
******
DRIFT, ALL SPOTS, SECOND 3RD OF APPARITION=
*****
DRIFTt ALL SPOTS, LAST 3RD OF APPARITION=
LIFETIME (DAYS), ALL SPOTS WITH DEFINITF OR PROBABLE LIFETIMES COMPUTED=
1.0
PROPORTION, ALL SPOTS=
LENGTH OF ALL SPOTS=
6.0
RATIO OF TYPICAL DEVIATIONS IN LENGTH TO LENGTH, ALL SPOTS,
(WEIGHTED)=
DISTRIBUTI-ON OF
LFNGTH=
N X LIFE=
N X LIF E =
0-
10-I11
0.0
0.0
SPnTS BY
3- 4
0.0
4- 5
0.0
5- 6
22.0
11-12
0.0
12-13
0.0
13-14
0.0
14-15
0.0
15-16
0.0
16-17
01. 0.
21-22
0.0
22-23
0.0
23-4
0.0
?4-25
25-26
26-27
0.0
0.0
0.0
OVAL
2
SLANT
_____________________________~
FESTOON
0
WAVE
2
OF SPOTS
ANGULAR
0
*****
0.17
(DEGREES)
2- 3
0.0
DISTRIBUTION
TYPE
NUMBER
LENGTH
1- 2
0.0
1
0.0
SLFNGTth=
.N X LIFE=
____
CURRENT
6-
7
o.0
8- 9
0.0
9-10
0.0
17-18
0.0
18-19
0.0
19-20
0.0
27-28
0.0
28-29
0.0
29-**
0.0
7- 8
0.0'
BY TYPE
AMORPHOUS
1
VARIABLE.
1
I
PREC.
7
END
FOL.
7
END
~C~
THE
FOR
30-DAY
DRIFT,
DRIFT,
DRIFT,
CRIFT,
DRIFT,
MEAN DR IFT,
ME AN DRIFT,
MEAN DRIFT,
MEAN OR IFT,
MEAN
MEAN
ME AN
MEAN
MEAN
MEAN
NTR
DEFINITE
30-DAY
DRIFT,
DRIFT,
ORIFT,
DRTFT,
DR I FT,
T4EAN DRIFT,
MEAN DRIFT,
DR IFT,
MEAN
DRIFT,
30-DAY
CRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DR IFT,
DRIFT,
AND PROBABLE
SPOTS
18.1
AV. DEV= 10.04
DRIFT,
ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
21.1
AV. DEV=
6.84
ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
20.3
AV. DEV=
8.33
2.48
23.4
AV. DEV=
LIGHT SPOTS (OVER 16 DAYS), UNWEIGHTED =
S'MALL SPOTS IUNWEIGHTFD) =
20.5
AV. DEV=
7.23
AV. DEV=
5.85
=
22. 1
LARGE SPOTS (UNWEIGHTED)
DARK SPOTS IWEIGHTED)=
16.7
AV. DEV= 11.30
LIGHT SPOTS (WEIGHTED)
=
23.4
AV. DEV=
3.52
SMALL SPOTS (WEIGHTED)
=
17.0
AV. DEV= 11.79
LARGE SPOTS (WEIGHTED)
=
19.7
AV. DEV=
7.38
FCR DEFINITE,
MEAN
MEAN
MEAN
MEAN
MEAN
MEAN
MFAN
MEAN
MEAN
MEAN
SPOTS
18.0
AV. DEV= 10.10
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
.71.2
AV. DEV=
6.74
ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
DARK SPOTS (OVER 10 DAYS).
UNWEIGHTED
20.6
AV. DEV=- 8.22
2.62
AV. OEV=
23,1
UJNWFIGHTED =
LIGHT SPOTS (OVER 10 DAYS),
AV. DEV=
6.93
=
20.8
SMALL SPOTS (UNWEIGHTED)
LARGE SPOTS (UNWEIGHTED)
=
22.3
AV. DEV=
5.82
DARK SPOTS (WEIGHTEO)=
16.6
AV. DEV= 11.24
DEV=
3.74
23.4
AV.
LIGHT SPOTS (WFIGHTED) =
SMALL SPnTS (WEIGHTED) =
17.6
AV. DEV= 11.21
7.26
=
19.9
AV. DEV=
LARGE SPOTS (WEIGHTFD)
FOR DEFINITE
MEAN
MEAN
ME AN
MFAN
' AN
MEAN
CURRENT
PRnRADBLE,
AND POSSIBLE
SPOTS
18.1
AV. DEV= 10.05
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
21.2
A V. DEV=
6.73
UNWEIGHTED =
ALL SPOTS (OBSVO LIVES 10 DAYS OR MORE),
AV. DEV=
20.4
8.19
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
EV= 2.48
UNWEIGHTED =
23.4
AV O.
LIGHT SPOTS (OVER 10 DAYS),
SMALL SPOTS (UNWEIGHTED) =
20.5
AV. DEV=
7.23
AV. DEV=
5.62
=
22.3
LARGE SPOTS (UNWEIGHTED)
r)EV= 11.29
16.7
AV.
DARK SPOTS (WFIGHTFD)=
3.52
AV. DEV=
=
23.4
LIGHT SPOTS (WEIGHTED)
SMALL SPOTS (WEIGHTED) =
17.0
AV. DEV= 11.79
LARGE SPOTS [WEIGHTED)
=
19.6
AV. DEV=
7.50
THE
FOR
MEAN
ME AN
MEAN
MFAN
MEAN
MFAN
MEAN
MFAN
MEAN
CURRENT
NTR
DEFINITE ANO
2.23
OF LONG-TERM DEVIATIONS FROM SPOTS' MEAN DRIFTS=
*****
OF TYPICAL SHORT-TERM DEVIATIONS IDEG.) FROM SPOTS' MEAN POSITIONS=
16.3
ORIFT, ALL SPOTS, FIRST 3RO OF APPARITION=
22.6
DRIFT, ALL SPOTS, SECOND 3RO OF APPARITION=
******
DRIFT, ALL SPOTS, LAST 3RD OF APPARITION=
88.2
LIFETIME (DAYS), ALL SPOTS WI.TH DEFINITE OR PROBABLE LIFETIMES COMPUTED=
2.2
PROPCRTION, ALL SPCTS=
****
LENGTH OF ALL SPOTS=
0.23
RATIO OF TYPICAL DEVIATIONS IN LENGTH TO LENGTH, ALL SPOTS, (WEIGHTED)=
DISTRIBUTION
:'IE NGT H=
N X LIFE=
0- 1
0.0
1- 2
0.0
2- 3
23.0
LENGTH=
IN X LIFE=
10-11
11-12
12-13
59.0
LE NG TH=N X L IFE=
20-21
0.0
22-23
0.0
5.0
15.0
21-27
0.0
OF
SPOTS
TYPE
NUMBER
OVAL
28
SLANT
FESTOON
0
WAVE
21
BY LENGTH
(DEGREES)
4- 5
2q6.5
5- 6.
663.0
6-,7
395*.0
7- 8
391.0
8-. 9
.297.0
9-10
58.5
13-14
0.0
14-15
0.0
15-16
0.0
16-17
46.0
17-18
71.0
-18-19
'0.0
19-20
0.0
23-24
0.0
24-25
0.0
25-26
0.0
26-27
0.0
27-28
0.0
28-29
0.0
29-**
0.0
3- 4'
63.0
DISTRIBUTION OF
L
PROBABLE SPOTS
ANGULAR
?
SPOTS BY TYPE
AMORPHOUS
19
VARIABLE
1
PREC. END
8
FOL, END
7-
_L
THE NNTBS CURRENT
FOR DEFINITE
SPOTS
4.82
AV. DEV=
-3.3
MEAN 30-DAY DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
5.76
AV. DEV=
-1.2
MEAN DRIFT,
ALL SPOTS (OSVD LIVES 10 DAYS OR MORE), UNWEIGHTED =
6.82
AV. DEV=
0.8
MEAN DRIFT, DARK SPOTS (OVER 10 DAYS) , UNWEIGHTED
4
AV. DEV=
-3.6
UNWEIGHTED =
MEAN CRIFT, LIGHT SPOTS (OVER 10 DAYS),
5.91
AV. DEV=
-1.2
=
MEAN DRIFT, SMALL SPOTS (UNWFIGHTED)
3.39
AV. DEV=
-4.3
=
MEAN DRIFT,. LARGE SPOTS (UNWEIGHTED)
4.89
AV. DEV=
-3.0
MEAN DRIFT, DARK SPOTS (WEIGHT.ED)=
4.36
AV. DEV=
-3.8
MEAN DRIFT, LIGHT SPOTS (WEIGHTED) =
6.22
AV. DEV=
-4.2
SMALL SPOTS (WE IGHTED) =
MEAN DRIFT,
2.85
AV. DEV=
-3.3
MEAN DRIFT, LARGE SPOTS (WEIGHTED) =
FOR
MEAN
MEAN
MEAN
ME AN
MMEAN
FAN
MEAN
MEAN
MEAN
MEAN
30-DAY
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DEFINITF AND PROBABLE SPOTS
4.82
AV. DEV=
-3.3
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS
5.76
DEV=
AV.
-1.2
UNWEIGHTED =
ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE),
6.82
AV. DEV=
0.8
UNWFIGHTED
DARK SPOTS (OVER 10 0AYS),
4.31
DEV=
AV.
-3.6
UNWEIGHTED =
LIGHT SPOTS (OVER 10 DAYS),
5.91
AV. DEV=
-1.2
=
SMALL SPOTS (UNWEIGHTED)
3.39
DEV=
AV.
-4.3
=
LARGE SPOTS (UNWEIGHTED)
4.89
AV. DEV=
-3.0
DARK SPOTS (WEIGHTED)=
4.36
AV. DEV=
-3.8
LIGHT SPOTS IWFIGHTED) =
6.22
AV. DEV=
-4.2
=
SMALL SPOTS (WEIGHTED)
2.85
AV. DEV=
-3.3
=
LARGE SPOTS (WEIGHTED)
FCR DEFINITE, PROBABLE, AND POSSIBLE
MEAN
MEAN
MEAN.
MEAN
ME AN
MEAN
MEAN
MF AN
MEAN
MEAN
_
SPOTS
4.82
AV. DEV=
-3.3
ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
5.76
DEV=
AV.
-1.2
=
UNWEIGHTED
DRIFT, ALL SPOTS (OBSVD LIVES 10 FAYS OR MORE),
6.82
DEV=
AV.
0.8
DRIFT, DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
4.31
AV. DEV=
-3.6
DRIFT, LIGHT SPOTS IOVER 10 DAYS), UNWEIGHTED =
5.91
DFV=
AV.
-1.2
=
DRIFT, SMALL SPOTS (UNWEIGHTED)
3.39
AV. DEV=
-4.3
=
DRIFT, LARGE SPOTS (UNWEIGHTED)
4.89
DEV=
AV.
-3.0
CRIFT, DARK SPOTS (WEIGHTEC)=
4.36
AV. DEV=
-3.8
=
DRIFT, LIGHT SPnTS (WEIGHTED)
6.22
DEV=
AV.
-4.2
=
DR IFT, SMALL SPOTS (WFIGWTFO)
2.85
DEV=
AV.
-3.3
=
DRIFT, LARGE SPOTS (WEIGHTED)
30-DAY DRIFT,
I _ 1
THE
NNTBS CURRENT
FOR DEFINITF AND
MEAN
MEAN
MEAN
ME AN
MEAN
ME AN
MEAN
MEAN
ME AN
SPOTS
2.06
OF LONG-TERM DEVIATIONS FROM SPOTS' MEAN DRIFTS=
3.43
OF TYPICAL SHORT-TERM DEVIATIONS (DEG.) FROM SPOTS' MEAN POSITIONS=
-6.6
DRIFT, ALL SPOTS, FIRST 3RD OF APPARITION=
-5.0
DRIFT, ALL SPOTS, SECOND 3RD OF APPARITION=
******
DRIFT, ALL SPOTS, LAST 3RD OF APPARITION=
*****
LIFETIME (DAYS), ALL SPOTS WITH DEFINITE OR PROBABLE LIFETIMES COMPUTED=
2.5
PROPORTION, ALL SPOTS=
6.1
LENGTH OF ALL SPOTS=
0.18
RATIO OF TYPICAL DFVIATIONS IN LENGTH TO'LENGTH, ALL SPOTS, IWEIGHTED)=
DISTRIBUTION OF SPOTS
'LENGTH=
N. X LIFE=
0- 1
0.0
BY LENGTH (DEGREES)
1- ?
0.0
2- 3
3.0
3- 4
46.0
4- 5
149.0
5- 6
92.0
6- 7
57.0
7- 8
142.0
8- 9
86.0
9-10
0.0
L.ENGT -=
"M X LIFE=
10-11
205.0
11-12
0.0
12-13
0.0
13-14
0.0
14-15
0.0
15-16
0.0
16-17
0.0
17-18
0.0
18-19
0.0
19-20
0.0
'tENGTH=
N X LIFE=
20-21
0.0
21-22
0.0
22-23
0.0
23-24
0.0
24-25
0.0
25-26
0.0
26-27
0.0
27-28.
0.0
28-29
0.0
29-**
0.0
DISTRIBUT ION OF
TY PF
NU MB E R
_
PROBABLE
OV AL
12
SL ANT FEST3V'
2
WAVE
2
ANGULAR
0
SP3TS BY TY3E
AMORP-IOUS
3
VARIABLE
0
PREC. END
7
FOL. END
7
I
1
~j
__
THE NNTEZ
CURRENT
FOR DEFINITE
MEAN
MEAN
MEAN
MEAN
MFAN
MEAN
MEAN
MEAN
MEAN
MEAN
30-DA Y
DRIFT,
DRIFT,
DR IFT,
ORIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
DRIFT,
-9.8
AV. DEV=
3.94
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE) , UNWEIGHTED =
-10.3
AV. DEV=
3.62
DARK SPOTS (OVER 10 DAYS),
UNWEIGHTED
-7.9
AV. DEV=
1.40
LIGHT SPOTS (OVER 10 DAYS), UNWEIGHTED =
-17.5
AV.
DEV=
0.0
SMALL SPOTS (UNWEIGHTED)
-17.5
AV. DEV=
0.0
LARGE SPOTS (UNWEIGHTED)
-10.0
AV. DEV=
0.0
DARK SPOTS (WEIGITED)=
-7.2
AV. DEV =
1.46
=
-17.5
AV. DEV=
0.0
LIGHT SPOTS (WEIGHTED)
SMALL SPOTS (WEIGHTED)
=
-17.5
AV. DEV=
0.0
AV. DEV=
0.0
=
-10.0
LARGE SPOTS (WFIGHTED)
FOR DEFINITE AND
4'
PROBABLE
SPOTS
4iE A N 30-DAY DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
-9.8
AV. DEV=
3.94
MEAN DRIFT, ALL SPOTS (OBSVD LIVES 10 DAYS OR MORE),
UNWEIGHTED
-10.3
AV. DEV=
3.62
MEAN ORIFT,
DARK SPOTS (OVER 10 DAYS),
UNWEIGHTED
-7.9
AV. DEV=
1.40
ME AN DRIFT, LIGHT SPOTS (OVER 10 DAYS),
0.0
UNWEIGHTED =
-17.5
AV. DEV=
FEAN DRIFT, SMALL SPOTS (UNWEIGHTED)
=
-17.5
AV. DEV=
0.0
MEAN DRIFT, LARGE SPOTS (UNWEIGHTED)
=
-10.0
AV. DEV =
0.0
MEAN ORIFT, DARK SPOTS (WEIGHTED)=
-7.2
AV. OEV=
1.46
MEAN DRIFT, LIGHT SPOTS (WEIGHTED)
=
-17.5
AV. DEV=
0.0
MEAN ORIFT, SMALL SPOTS (WEIGHTFD) =
-17.5
AV. DEV=
0.0
MEAN DRIFT, LARGE SPOTS (WEIGHTED)
=
-10.0
AV.
DEV=
0.0
FOR DEFINITE, PROBABLE,
MEAN 30-DAY
MEAN DRIFT,
MEAN ORIFT,
MEAN DRI FT,
MEAN DRIFT,
MEAN DRIFT,
MEAN 'DRIFT,
ME AN DRIFT,
MEAN DRIFT,
MEAN CRIFT,
I_
SPOTS
AND POSSIBLE SPOTS
AV. DEV=
3.94
-9.8
DRIFT, ALL SPOTS, WEIGHTED BY NO. OF OBSERVATIONS =
ALL SPOTS (O0SVD LIVES 10 DAYS OR MORE),
UNWEIGHTED =
-10.3
AV. DEV=
3.62
DARK SPOTS (OVER 10 DAYS), UNWEIGHTED
-7.9
AV. DEV=
1.40
LIGHT SPOTS (OVER 10 DAYS), UNWFIGHTFD :
-17.5
AV. DEV=
0.0
SMALL SPOTS (UNWEIGHTED)
=
-. 17.5
AV.
DEV=
0.0
LARGE SPOTS (UNWETGHTFD)
=
-10.0
AV. DEV=
0.0
DARK SPOTS (WEIGHTED)=
-7.2
AV. DEV=
1.46
LIGHT SPOTS (WEIGHTED) =
-17.5
AV.
DEV=
0.0
SMALL SPOTS (WEIGHTED)
=
-17.5
AV.
DEV=
0.0
LARGE SPOTS (WEIGHTED)
=
-10.0
AV. DEV=
0.0
THE NNTFZ
CURRENT
FCR DEFINITE AND PROBABLE SPOTS
MEAN
MEAN
MEAN
MEAN
MEAN
MFAN
ME AN
MEAN
MEAN
CF LONG-TERM DEVIATIONS FROM SPOTS' MEAN DRIFTS= *****
2.50
OF TYPICAL SHORT-TERM DEVIATIONS (DEG.) FROM SPOTS' MEAN POSITIONS=
******
DRIFT, ALL SPOTS, FIRST 3RD OF APPARITION=
******
CRIFT, ALL SPOTS, SFCONO 3Ro OF APPAPITION=
****
DRIFT, ALL SPOTS, LAST 3RD OF APPARITInN=
*****
LIFETIME (DAYS), ALL SPOTS WITH DEFINITE OR PROBABLE LIFETIMES COMPUTED=
2.O
PROPORTION, ALL SPOTS=
6.5
LENGTH OF ALL SPOTS=
0.05
RATIO OF TYPICAL DFVIATIONS IN LFNGTH TO LENGTH, ALL SPOTS, (WEIGHTED)=
DISTR IRUTION
LENGTH=
N X LIFE=
0-
1
0.0
1- 2
0.0
2- 3
0.0
OF
SPOTS BY LENGTH (DEGREES)
4- 5
53.0
3- 4
0.0
0.0
0.0
7- 8
12.0
8- 9
0.0
9-10
0.0
5-
6-
6
7
LENGTH=
40 X L IFE=
10-11
0.0
11-12
0.0
12-13
0.0
13-14
0.0
14-15
0.0
15-16
0.0
16-17
0.0
17-18
0.0
18-19
0.0
19-20
0.0
t E NG T H=
N X LIFE=
20-21
0.0
21-22
0.0
22-23
0.0
23-24
0.0
24-25
0.0
25-26
0.0
26-27
0.0
27-28
0.0
28-29
0.0
29-*
0.0
DISTRIRUTION
TYPE
NUMBER
OVAL
3
SLANT FESTOON
0
WAVE
?
OF
ANGULAR
0
SPOTS BY TYPE
AMORPHOUS
2
VARIABLE
0
PREC.
7
END
FOL.
7,
END
1
APPEBDIX B
Tabulations of All Observed Spots
Note:
Tabulations for definite-and-probable and for definite-probable-
possible spots are omitted in this appendix in those cases when they are
identical to the tabulations which would have immediately preceded them
(i.e. when there are no additional probable or possible spots)..
THE NEBZ
CURRENT. NOV
DEFINITE
SPOT
44
45
46
47
48
49
50
51
52
53
54
55
57
58
59
60
61
62
63
64
65
66
67
68
69
70
71
72
73
74
75
76
*1
DATES OBSVD
81
89
89
103
103
103
113
121
128
126
121
140
145
151
159
1?1
121
713
143
114
165
5
30
41
58
71
58
80
11
27
11
76
91
185
91
90
104
104
104
113
121
130
130
128
140
145
151
161
128
128
128
186
143
184
19
32
43
66
90
65
90
15
76
73
83
91
LONG
42.
121.
129.
141.
135.
122.
148.
104.
180.
NO.
27
3
2
2
2.
2
1
1
2
3
3
DRIFT
-17.6
-165.0
-150.0
-60.0
-30.0
0.0
-30.0
7.5
-34.3
4*4*
3
2
2
8
9
4
3
2
2
2
6
2
4
2
12
13
5
SPOTS
ROT PERIOD
D,L
S
-120.0
-30.0
-18.6
-47.1
-18.8
-30.0
-12.6
-6.4
-45.0
0.0
-11.2
-7.9
-21.4
-12.0
-15.0
-12.2
-16.5
-90.0
4
4
3
3
3
3
3
2
2
2
2
2
3
3
0
3
2
2
2
3
2
2
.3
3
2
2
2
2
9H54M59.5S
9H55M50. 9S
9H54M 53.7S
*H**M***-* S
9H52M56.3S
9H54M59.5S
9H54M4 7 .-8S
9H54M36. IS
9H55M14.8S
9H54M59.5S
9H95M23. 3S
9H55M31.8S
9H54M39. OS
9H55'44 0.6 S
9H55M?5.2S
9H55M29.8S
9H55M I .3S
91155M24.2S
9H55M?O. IS
9H55M23.8S
9H55MIS. IS
9H53M3 7.4S
*H *,*M****S
P
1
3
2
9H55M16.5S
9H51M54.7S
9H52M15.3S
9H54M18.5S
9H54M59. 5S
9H55M40.6S
*H**M****S
*H**M*,*** S
1
344.
195.
212.
233.
181.
275.
247.
197.
130.
198.
185.
178.
167.
167.
?60.
261.
273.
318.
1967.
*H**M****S
1
1
2
1966-JUNE
2
2
1
T
0
0
0
4
4
1
4
4
4
0
3
3
0
0
4
4
0
0
6
0
0
4
0
0
4
0
0
5
0
0
0
4
4
LENGTH
12.5
5.0
4.0
7.0
4.0
2.0
3.0
4.0
3.0
3.0
3. 5
5.0
5.0
5.0
5.0
5. 5
4.0
.3.5
5.5
7.0
13.5
5.0
4.0
7.5
4.0
4.0
3.0
8.5
6.0
5.5
7.0
12.0
DL/L
0.36
0.0
0. 0
0.0
0.0
0.0
0.0
0.0
0.0
0.33
0.14
0.0
0.0
0.0
0.20
0.27
0.25
0.14
0.27
0.0
0.11
0.0
0.0
0.07
0.25
0.25
0.33
0.06
O. 17
0.27
0.14
0.0
DEV
3
*4
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*4
*4
*4
*4
*4
*
*
*4
*4
*4
*4
*4
*
*4
*4
*4
*4
*
2
*4
_
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44**4
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*
*
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*
***
***4
****
**44
44*444
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91
98
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--
*
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**
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******.
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**
0.0
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4*****
444444
**44*
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***
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(CONTINUED)
LIFFTIME
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WHY
TEXT)
2.
2.
7.
29.
7.
7.
2.
2.
29.
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NO.
59
54
51
4?
52
19
10
7
7
7
37
3
7
13
25
4
30
2
40
4
14
35
2
2
9
2
3
16
9
2
1
DRIFT
1966-JUNE 1967.
SPOTS
ROT PERIOD
-11.9
-12.1
-14.2
9f155M24.3S
-16.0
9HS5MI8.7S
9H55M25.3 S
9H55M17.1S
9H55M18.3S
9H55M33.IS
9H55M21.2S
9H55M36. OS
-11.2
-17.1
-16.3
-5.5
-14.7
-3.3
-13.1
-50.0
-13.9
-15.7
-13.4
-24.0
-6.?
-8.3
-20.0
9H55M24.0S
9H55M?1. 2S
9H55M22.7S
9H54M32.2S
9H55M21.6S
9H55M9.2S
9H55M22.2S
9H55M 7.8S
91H55M32. ?S
9H55M29.3S
9H55M 132S
-14.9
-15.9
9H55M20 .2S
-21.0
9H55MI .8S
9H55M20.6S
-14.6
-15.0
-17.1
-7.7
0.0
-8.2
-7.1
-14.2
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0.0
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9H55M 18.9S
9H55M20. S
9H55M17.IS
9H55M30. 0S
9H55M40. 6S
9H55M29.4S
9H55M30. 9S
9H55M21 .?S
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D,L
2
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21
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4
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LENGTH
DL/L
3.5
10.5
3.5
11.5
6.5
6.5
5.5
0.43
0.24
0.43
0.22
0.23
0.23
0.27
4.5
8.5
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5.0
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6.5
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4.5
5.5
4.5
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3.0
3.0
5.0
6.0
4.0
3.0
6.0
4.0
0. 11
0.18
0.25
0.0
0.10
0.20
0.23
0.0
0.0
0.14
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2
2
1
I
2
3
2
1
3
3
3
3
2
1
1
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3
0.33
0.14
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0.33
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DATES OBSVD
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15
88
15
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282.
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DRIFT
-10.0
(CONT INUED)
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9H55M26.9S
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S
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T
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35
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300EV
******
******
******
******
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******
*****
*****
_
(CONTINUED)
LIFETIM
******************
******C*************
(SEE TEXT)
WHY
PART
DATES
1,1
****
***-***
***-***
5,5
****
***-***
***-***
PROMINENT
1
THE NEBN
CURRENT. NOV 1966-JUNE
DFF INITF AND
SPOT
1
2
3
4
5
6
7
8
9
10
13
14
15
16
17
18
19
22
23
28
29
30
31
32
33
34
35
211
212
213
214
DATES
OBSVD
1 220
105
9 221
69 .202
2 219
6
72
11 46
123 145
171 190
94 130
34 75
5
72
36 181
140 150
140 208
76 225
73 76
1 78
182
193 204
127 220
120 158
172 174
173 175
104 104
82 88
15 15
2 203
1 225
11 37
127 175
LONG
6.
28.
40.
48.
89.
85.
82.
61.
73.
92?.
127.
133.
143.
215.
192.
220.
252.
273.
305.
327.
329.
352.
202.
287.
282.
120.
269.
321.
332.
NO.
59
54
51
42
52
19
10
7
7
7
7
13
25
4
11
30
2
14
35
.3
16
9
2
2
1.
2
1
40
44
4
11
DRIFT
-11.9
-12.1
-14.2
-16.0
-11.7
-17.1
-16.3
-5.5
-14.2
-3.3
-13.9Q
-15.7
-13.4
-24.0
-6.2
-8.3
-20.0
-21.0
-14.6
-8.2
-7.1
-14.2
-15.0
0.0
PRnBABLE
ROT
PERIOD
9H55M24.3S
9H55M24.0S
9H55M2 1. ?S
9H55M 8.7S
9H55M25.3S
9H55M17. 1S
9H55M18.3S
9H 55M33.1 S
9H55M21.2S
9H55M36.OS
9H55M21.6S
9H55Ml9.2S
9H55M?2.2S
9H55M 7.8S
9H55M32.2S
9H55M29. S
9H55M 13. 2S
9H551 I .8S
9H55M20.6S
9H55M29.4S
9H55M30. 9S
9H55M21.2S
9H55M20. 1S
9H 55M40. 6S
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-10.0
9H55M?6.9S
S
9H55M20.4S
9H55M20.4S
9H55M?1.7S
9HS5M24.4S
*H**M****
-14.8
-14.7
-13.8
-11.9
1967.
SPOTS
D,L
S
3
1
3
1
2
2
2
I1
1I
2
1
2
2
3
3
3
3
2
3
2
2
1
2
2
2
3
I
2
2
2
P
2
2
3
2
3
2
3
0
3
2
3
3
2
3
3
3
3
2
3
2
3
2
3
3
2
3
2
1
1
I
1
T
LENGTH
DL/L
3.5
0.43
0.24
0.43
0.22
0.23
0.23
0.27
10.5
.3.5
11.5
6.5
6.5
5.5
4. 5
8.5
10.0
7.5
6.5
3.0
3.0
3.5
3.0
5.5
4.5
5.0
6.0
4.0
3.0
6.0
4.0
2.5
2.0
7.5
5.0
3.5
3.0
0.11
0.18
0.10
0.20
0.23
0.0
0.0
0.14
0.0
DEV
2
2
I
1
2
3
2
3
3
3.
2
1
0.45
0.33
0.20
2
3
0.33
0.25
0.0
0.0
0.0
0.20
0.0
0.33
2
0.40
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0.0
1
1
2.
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I
I _1 _
THE NTRZ
CURRENT.
NOV
DEFINITE
SPOT
36
37
38
39
40
41
42
43
DATES OBSVD
2
16
70
104
121
158
103
145
9
16
70
104
139
158
103
145
LONG
12,.
NO.
DRIFT
-21.4
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**
76.
**** ~
• -11.7
* * *
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1967.
SPOTS
PERIOD
9H55M i.3S
*H**M****S
**
****
9
****
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ROT
1966-JUNE
*H**M****S
9H55M24.6S
*M*
H*M** * * S
*H*'*M****S
D,L
S
P
T
DL IL
DEV
5.5
0.09
7.0
2.0
5.0
11.0
6.0
2.0
.4,0
0.0
0.0
0.0
0,09
0,0
0.0
0.0
**
**
**
LENGTH
4*'
*
*4
**
**le
__
j
NTRZ
SPOT
(CONTINUFD)
DRIFTi
DRIFT2
ORIFT3
30DEV
LIFFTIME
36
37
*****
******
*****
******
*****
**C**
******
38
39
******
******
******
******
******
*****4
40
******
******
******
*****
**************
41
42
43
******
******
******
******
******
**1***
******
******
(SEE TEXT)
******
************
********************
7.
*****
*****
*****'*t**************
1.
*****
********************
1.
WHY
PART
DATES PROMINENT
9,2
2,1
5,2
5,5
215
215
****
****
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****
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18.
*****
********************
1.
*****
*****
********************
*******************
1.
11
1. 0**** 1,5
_
THE
NTRZ
__
CURRENT. NOV
DEFINITE AND
SPOT
38
39
40
41
42
43
215
DATES OBSVD
70
104
121
158
103
145
LONG
NO.
DRIFT
1966-JUNE 1967,
PROBABLE SPOTS
ROT PER IOD
70
104
139
.158
103
145
16
2
S
9H1155M24.6S
*H **M***
76.
-11 .7
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29.
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___
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D,L
S
P
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LENGTH
2.0
5.0
11.0
6.0
2.0
4,0
6.0
DL/L
0,0
0.0
0.09
0.0
0.0
0.0
0.17
DEV,
**~t
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_
NTR7
(CONTINJED)
DRIFT1
DRIFT2
DRIFT3
300DEV
38
******
******
******
*****
,**********c**;******
39
40
******
******
******
******
******
******
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*****
********'********
***********
**-****
41
******
******
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*****
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1.
42
43
******
******
******
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j.
1, 1
1,5
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******
******
*****
******
9,1
****
SPOT
215
WAY
PART
DATES
1,
5,2
1.
5,5
1,1
****
****
****
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LIFETP4E (SEE TEXT)
******'**
18.
l*
?8.****
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c***
PROMINENT
**-***
***-***
**,*-***
******
***-***
***-***
***-***
***-***
***-***
***-***
***-***
THE NTBS
CURRENT. NOV 1966-JUNE 1967.
DEFINITF
SPOT
190
DATES OBSVD
5
27
LONG
319.
NO.
ORIFT
4
3?,7
ROT
SPOTS
PERIOD
9H56M25.4S
DL
2
S
?
P
1
T
5
LENGTH
6.0
DL/Lt
0.17
DEV
NTfS
SPOT
(CONTINUED)
DRIFTI
DRTFT2
DRIFT3
3 ODFV
LIFETIME
190I~arlO~a
I~~r~k~
t~f~~d
Jefi~It
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(SEE
TEXT)
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WHY
1
PART
DATES PROMINENT'
~c~~lelc~~4l S~e~~s~~
THE NTB
CURRENT.
NOV
1966-JUNE
_
~___
_I
_
1967.
DEFINITE SPOTS
SPOT
101
102
103
104
105
106
107
108
109
110
All
112
113
114
115
116
17
1 18
119
120
121
12?
123
124
125
126
127
128
129
130
131
132
133
DATES OBSVD
52
37
52
47
69
60
78 .79
82
80
87
72
94
88
87 160
172 174
186, 196
46 49
30
28
16
6
49
28
58
58
80
65
82
82
87 104
113 186
13
6
16
11
21
1
65
35
77
50
82
72
96
65
72 104
79 130
143 160
96
7
28 110
90
77
2
28
LONG
60.
43.
72.
59.
63.
34.
23.
41.
137.
32.
57.
32.
66.
71.
***
86,
*4*
86.
89.
82.
99.
108.
112.
140.
144.
90.
96.
67.
53.
158.
165.
177.
178.
NO.
6
3
4
?
2
9
0
15
2
3
3
2
6
11
1
6
1
6
14
4
4
9
7
5
4
10
11
13
4
23
20
6
7
DRIFT
34.0
6.0
40.0
30.0
15.0
22.0
20.0
31.6
0.0
33.0
10.0
0.0
18.0
18.6
28.0
*4**4*
21.2
20.5
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154
156
157
158
159
160
161
162
165
166
167
168
169
170
171
172
173
174
175
176
177
178
179
180
181
182
183
184
185
186
187
DATES
37
69
64
64
30
64
1
15
115
113
113
122
209
166
130
171
121
121
160
160
121
165
121
121
171
140
114
104
120
144
139
132
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88
73
202
134
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43
105
79
20
152
212
183
181
209
181
152
155
160
155
184
184
174
174
140
131
1.84
158
175
134
146
173
185
144
LONG
313.
336.
327.
341.
354.
357.
355.
348.
285.
4.
351.
339.
340.
330.
23.
55.
79.
110.
97.
100.
115.
126.
119.
88.
170.
152.
210.
222.
226.
230.
263.
309.
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14
3
36
24
3
3
19
24
2
14
25
17
15
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6
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5
6
11
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(CONT INUED)
ROT PERIOD
D,L
P
S
25.3
30.0
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12.0
13.8
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0.0
30.0
30.8
0.0
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30.5
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9H55M40.6S
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2
3
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9H56M13.3S
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9H56M11.4S
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9H56M28.?S
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9H55M56.3S
9H56M21.7S
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23
2
5
4
9
6
12
34.7
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28.0
4
5
8
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31.2
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LENGTH
8.5
2.5
6.5
6.5
11.0
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0.29
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0.20
0,23
0.23
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0.30
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11.5
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188
189
223
224
225
226
227
228
229
230
DATES
103
193
87
6
58
79
65
5
49
127
OBSVD
166
209
196
49
186
160
175
19
110
188
LONG
302 .
215.
41.
74.
87.
67.
188.
261.
265.
348.
~_~_~
NO.
13
4
20
17
28
17
13
3
14
9
___
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ICONTINUED)
DRIFT
ROT PERIOD
19.95
20.6
30.8
20.9
22.7
28.1
21.8
23.6
24.6
17.2
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9H56M22. 8S
9H56M 9.3S
9H56M1 1.7S
9H56M19. IS
9H56MI0.5S
9H56M12.9S
9H56M14.3S
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0
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LENGTH
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DL/L
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5
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1
2
3
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6.0
0.33
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1
1
2
2
2
0
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SPOT
188
189
723
224
225
2?6
227
228
229
230
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3.11
0.0
1.11
0.0
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0.0
0.0
1
___
_ ____
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(CONTINUEO)
LIFETIME (SEE TEXT)
WHY
1,0
3,9
0, 9
*4****************** 43.
9,3
******4*44******
128.
3,3
4*****************
4, 3
8.
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9,5
*******4***********
~61.
1, 1
8,9
****************2.****
PART
DATES
* * *-
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********************
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********
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CURRFNT. NOV
DEFINITE, PROBABLE,
SPOT
101
107
103
104.
105
106'
107
ll
'112
120
,121
122
123
124
125
126
130
131
132
133
136
137
138
143
144
145
146
150
151
1 52
153
1.54
DATES OBSVD
37
52
47
52
60 S69
78 79
80 82
72 87
88 94
46
49
28 30
6
13
16
11
1 21
35 65
77
50
72 8?
65 96
72 104
96
7
28 110
90
77
28
2
104 175
36
95
87 95
37
58
76 202
76
80
71
5
5
69
37
69
134
225
39
105
88
73
tONG
60.
43.
72.
59.
63.
34.
23.
5.7.
32.
82.
99.
108.
11?.
140.
144.
90.
96.
158.
165.
177.
178.
200.
226.
242.
265.
245.
255.
257.
219.
283.
290.
313.
336.
NO.
DRIFT
6
3
4
2
34.0
6.0
40.0
30.0
15.0
22.0
9
0
3
2
4
4
9
7.
5
4
10
11
23
20
6
7
11
11
3
6
26
2
19
43
6
8
14
20.0
10.0
0.0
17.1
30.0
19. 5
24.0
22.2
33.0
25.2
26.2
25.6
24.1
23.1
23.1
22.0
22.9
11.?
34.3
24.0
.45.0
22.4
0.0
22.1
16.7
25.3
30.0
ROT
I_~_
1966-JUNE 1967.
AND POSSIBLE SPOTS
PERIOD
D,L
2
1
1.
1
2
2
.2
9H56M27.2S
9H55M48.8S
9H56M35.4S
9H56M1?.
7S
9H56M 1.1S
9H56M10.7S
9H56 4 8.OS
9H55M54. 3S
9H55M40.6S
9H56M 4.1 S
9H56M21.7S
9H56M 7.3S
9HS6MI3.5S
9H56M11 .OS
9H56M25.8S
9H56M 5.1 S
9H56MI6.6S
9U56M1 5.7S
9H56M13.7S
9H56MI2.2S
9H56MI2.2S
9H56M 10. 7S
9H56M11.9S
9H55M56.0S
1
I
2
2
1
9 H 56M27.6
9H56M13.5S
9H56M42. ?S
9H56M1 1.2S
9H55M40. 6S
9H56M10. 8S
9H56M 3.45
9H 56M1 5. 2 S
9H56M?1. 7S
1
P
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2
2
1
2
2
2
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3
2
2
2
2
2
2
1
2
2
1
2
2
2
2
3
3
3
0
2
2
0
3
3
2
1
2
3
3
3
3
3
2
1
2
2
0
3
2
2
2
2
2
2
3
T
2
2
2
2
3
0
7
0
4
7
0
4
4
5
0
0
4
2
4
0
2
0
2
0
7
2
0
0
2
0
0
2
2
LENGTH
DL/L
5.5
0.27
9.0
7.0
4.0
3.0
6.0
0.11
6.5
6.5
0. 23
0.23
5.0
0.20
7.5
8.0.
9.5
3.5
5.5
6. 5
4.5
6.0
2.5
9.0
18.0,
12.5
4.5
0.33
0. 0
7.5
3.0
5.5
6.0
7.5
5. 0
8.5
2.5
~C
DEV
0.43
0.0
0. 0
0.17
0.26
0.14
0.27
0.23'
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9H56M21.7S
9H56M22.8 S
9H 55M40. 6S
9H55M40.6S
9H56M35.4S
9H56M2 1.7S
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9H56M 13.3S
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9H55M57.7S
9H56M 7.35
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9H56M22.8S
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PFRIOD
9H56,M 12.9S
9H56M14.3S
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9H'55M58.?S
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D,L
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P
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2
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4
2'
LENGTH
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DEV
3. 5
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7.5
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6.5
0.14
0.33
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THE
NNTBS
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NOV
DEF INITE
SP3T
191
19'2
193
194
195
196
197
198
199
200
701
202,
203
204
205
DATES 03SV)
17
3
88
104
126
127
2
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28
130
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21
208
182
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31
159
152
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16
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10.3
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ROT
1966-JUNE
1967.
SPOTS
PE RI OD
9H55M 9.8S
9H55M38.0S
9H55M30.6S
9H5SM40.6S
9H55M q. 8S
9H55M56.6S
9H55M40.6S
9H55M31.6S
9H55M54.3S
9H55M54. 8S
9H55M42. OS
9H55M44.?S
9H55M1. 1 S
9H55M29.9S
9H55M29. 5S
D,L
S
P
T
LENGTH
DL/L
DEV
3.5
10.5
8.0
9.0
5.0
0. 14
0.33
0.13
0.11
0.0
6
4
0
6.0
5.0
3.0
4.0
6.0
7.0
4.0
6.0
8.0
0.0
0.20
0.0
0.0
0.0
0.14
0.25
0.17
0.25
3
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5
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NOV
DEFINITE
SPOT
206
207
208
209
210
DATES OBSVD
58 77
19
28
83 140
121. 174
132 144
LONG
131.
76.
99.
173.
271.
NO.
3
3
8
6
4
DRIFT
-
-7.9
-6.7
-5.8
-17.5
-10.0
1966-JUNE
_ _
1967.
SPOTS
ROT PERIOC
9H55M29.8S
9H.55M31 . 5S'
91 55,M 2. 7S
9H155M16.6S
9H55M?6.9S
D,L
T
P
S
LENGTH
DL/L
0
6
****
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0
7
****
****
0
6
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0
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8.0
0.13
DEV
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NNTEZ
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******
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******
206
***
207
******
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20
209
210
******
**(***
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*****
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s
_
(CONTINUED)
LIFETIMF
30DEV
~ ~ ~___
__
(SEE
TEXT)
*****
***
*****
****************
19.
9.
*******************
******************
******************
57.
53.
12.
0.0
0.0
****
*4*C************
I
WHY
PART
DATES PROMINENT
22
****
***-***
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2,2
****
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****
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2,2
/
_
APPEtDIX- 0
Relationships Between Spot Characteristics
115
I __/I
_
SPOTS
DARK
N= 16.
2.12
MEAN LONG-TERM DEVIATIONS FRCM MFAN DRTFTS=
*****I:
FROM MEAN POSITIONS=
'MEAN SHORT-TERM DEVIATIONS (DEG.)
N= 19.
103.4 DAYS
MEAN CF DEFINITE fR PRCOABLE LIFETIMFS=
N= 78.
2.5
MEAN PROPORTION=
N= 78.
6.4
MEAN LENGTH=
N= 78.
0.16
MEAN RATIO OF LENGTH-DEVIATION Tn LENGTH=
MEAN SIGNED DEVIATION OF DRIFT FROM CURRENT MEAN {NEG=SLOW)
9.3
NUMBER OF DARK SPOTS=
0
NUMBER OF LIGHT SPOTS=
DISTRIBUTION
4"
TYPE
NUMBER
OVAL
22
SLANT
FESTOON
4
WAVE
21
~_
_~ _
_ _~ i ___grr~l~_~____i ~_~_
N= 32.
1.41
N= 67.
OF SPOTS BY TYPE
ANGULAR
4
AMORPHOUS
31
+
VARIABLE
0
PREC.
5
END
FOL.
6
END
~__
__
ii
I
~
1_ _
I
SPOTS
LIGHT
N= 14.
1.98
MEAN LnNG-TFRM DEVIATIONS FRCM MEAN. DRIFTS=
N=
*****
FROM MEAN POSITIONS=
MEAN SHORT-TERM DEVIATIONS (DEG,)
N= 13.
93.0 DAYS
MEAN CF DEFINITE OR PROBABLE LIFETIMES=
N= 85.
2.1
MEAN PROPORTION=
N= 85.
****
MEAN LENGTH=
N= 85.
0.17
MEAN RATIO CF LENGTH-DEVIATION TO LENGTH=
-2.05
MEAN SIGNED DEVIATION OF DRIFT FROM CURRENT MEAN INEG=SLOW)
0
NUMBER OF DARK SPOTS=
87
NUMBER OF LIGHT SPOTS=
DISTRIBUTION
wwe
TYPE
NUMBER
OVAL
65
SLANT
FESTOON
0
WAVE
7
27.
N= 46.
OF SPOTS BY TYPE
ANGULAR
0
_
n
AMORPHOUS
14
I
VARIABLE
4
PREC. END
1
FOL. END
I
_li ~ ~~___~__
10 DEG
SPOTS OVER
LONG
6.
N=
3.36
MEAN LONG-TERM DEVIATIONS FROM MEAN DRIFTS=
N=
2.57
MEAN SHORT-TERM DEVIATIONS (rEG.) FROM MEAN POSITIONS=
3.
N=
DAYS
170.0
MEAN OF DEFINITE OR PROBABLE LIFETIMES=
N= 12.
1.3
MFAN PROPORTION=
N= 12.
****
MEAN LENGTH=
N= 12.
0.18
MEAN PATIO OF LENGTH-DEVIATION TO LENGTH=
-0.36
(NEG=SLOW)
MEAN
CURRENT
MEAN SIGNED DEVIATION OF DRIFT FROM
5
NUMBER OF DARK SPOTS=
7
NUMBER CF LIGHT SPOTS=
DISTRIBUTION
,': TYPE
NUMBER
OVAL
6
SLANT
FESTOON
0
WAVE
1
OF
ANGULAR
0
SPOTS
7.
N=
10.
BY TYPE
AMORPHOUS
4
VARIABLE
0
PREC.
1
END
FOL.
0
END
j__
_____
SPOTS 5
Tr
10
DEG LONG
N= 15.
1.53
MEAN LONG-TERM DEVIATIONS FRCM MEAN DRIFTS=
N= 36.
*****
FROM MEAN POSITIONS=
MEAN SHORT-TERM DEVIATIONS (DEG.)
N= 18.
90.4 DAYS
MEAN OF DEFINITE OR PROBABLE LIFETTMES=
N=101.
2.2
MEAN PROPORTION=
N=101.
6.8
MEAN LENGTH=
N=101.
0.18
MEAN RATIO OF LENGTH-DEVIATION TO LENGTH=
N= 71.
MEAN SIGNED DEVIATION OF DRIFT FROM CURRENT MEAN (NEG=SLOW) -0.12
52
NUMBER OF DARK SPOTS=
49
NUMBER OF LIGHT SPOTS=
DISTRIBUTI ON OF
TYPE
NUMBER
OVAL
51
SLANT FESTOON
1
WAVE
15
ANGULAR
0
SPOTS BY TYPE
AMORPHOUS
31
VARIABLE,
3
PREC.
0
END
FOL.
0
END
.'4-:
~:
V
_1
SPOTS LESS THAN
5
OEG LONG
5.
1.76
N=
MEAN LONG-TERM DEVIATIONS FRCM MEAN DRIFTS=
*****
N=
FROM MEAN POSITIONS=
MEAN SHORT-TERM DEVIATIONS (DEG.)
4.
N=
130.9 DAYS
MFAN OF DEFINITE OR PROBABLE.LIFFTIMES=
MFAN PROPORTION=
2.7
N= 50.
MEAN LENGTH=
3.4
N= 50.
0.12
N= 50.
MEAN RATIO CF LENGTH-DEVIATION TO LENGTH=
-2.22
MEAN SIGNED DEVIATION OF DRIFT FROM CURRENT MEAN {NEG=SLOW)
NUMBE'R OF DARK SPOTS=
21
?7
NUMBER OF LIGHT SPOTS=
DISTRIBUTION
TYPE
NU MBE R
OVAL
28
SLANT
FESTOCN
3
WAVE
5'
9.
N=
18.
OF SPOTS BY TYPE
ANGULAR
4
AMORPHOUS
9
VARTABLE ,
1
PREC.
0
END
FOL.
0
END
'-t
,-1
1~~__
_ ~__)
__
TALL
____~_
SPIOTS
0.
N=
*'~**
MEAN LONG-TERM DEVIATIONS FROM MEAN DRIFTS=
N=
*****
POSITIONS=
MEAN
FROM
(DEG,)
DEVIATICNS
SHORT-TERM
MEAN
0.
N=
DAYS
':****
LIFETIMES=
PROBABLE
OR
MFAN OF DEFINITE
5.
N=
4.0
MEAN PROPORTION=
5.
N=
3.7
MFAN LENGTH=
5.
N=
0.03
MFAN RATIO OF LENGTH-DEVIATION TO LENGTH=
MEAN SIGNED DEVIATION OF DRIFT FROM CURRENT MEAN (NEG=SLOW) *****
5
NUMBER OF DARK SPOTS=
0
NUMBER OF LIGHT SPOTS=
0.
N=
0.
DISTRIBUTION OF SPOTS BY TYPE
TYPE
NUMB ER
OVAL
0
SLANT FESTOON
4
WAVE
0
ANGULAR
0
AMORPHOUS
1
--
VARIABLE
0
PREC. END
0
FOL. END
0
__
___
RGUND
SPOTS
9.
N=
1.46
MEAN LONG-TERM DEVIATIONS FROM MFAN DRIFTS=
N=
2.44
POSITIONS=
MEAN
FROM
(DEG.)
DEVIATIONS
MEAN SHORT-TERM
11.
N=
DAYS
115.0
LIFETIMFS=
PROBABLE
OR
MFAN OF DEFINITE
N= 59.
3.0
MEAN PROPORTION=
59.
N=
4.9
MEAN -LENGTH=
N= 59.
0.16
TO LENGTH=
LENGTH-DEVIATION
OF
MEAN RATIO
-0.3q
(NEG=SLOW)
MEAN
CURRENT
FROM
DRIFT
OF
DEVIATION
MEAN SIGNED
29
SPOTS=
DARK
OF
NUMBER
30
NUMBER OF LIGHT SPOTS=
DISTRIBUTION
TYPE
NU MB ER
OVAL
33
SLANT FESTOON
0
WAVE
5
16.
N=
30.
OF SPOTS BY TYPE
ANGULAR
3
AMORPHOUS
17
VARIABLE
1
PREC. END
0
c
FOL. END
,
0
.
_
I
I
/_
.1
SPOTS
LONG
MEAN LONG-TERM DEVIATIONS FROM MEAN DRIFTS=
1.92
N* 10.
N= 23.
MEAN SHORT-TERM DEVIATIONS (DEG.)
FROM MEAN PnSITIONS=
2,78
MEAN OF DEFINITE OR PRORABLE LIFFTIMES=
109.2 DAYS
N= 12.
N= 73.
2.0
MEAN PROPORTION=
MEAN LENGTH=
6.6
N= 73.
MEAN RATIO OF LENGTH-DEVIAT ION TO LENGTH=
0.15
N= 73.
N= 45.
MEAN SIGNED DEVIATION OP DRIFT FROM CURRENT MEAN (NEG=SLOW)
1.07
41
NUMBER OF DARK SPOTS=
NUMBER OF LIGHT SPOTS=
37
DISTRIBUTION
TYPE
NUMBER
OVAL
38
SLANT
FESTO1ON
0
WAVE
14
OF
ANGULAR
0
SPOTS BY TYPE
AMORPHOUS
20
VARIABLE
1.
PREC.
0
END
FOL.
0
END
li_
___
_
VERY LONG SPOTS
N=
7.
2.79
MEAN LONG-TERM DEVIATTIONS FROM MEAN DRIFTS=
MEAN SHORT-TERM DEVIATIONS (DEG.) FROM MEAN POSITIONS=
*****
N=
MEAN OF DEFINITE OR PROPABLE LIFETIMFS=
42.5 DAYS
N=
2.
MEAN PROPORTION=
1.0
N= 26.
N= 26.
***,
MEAN LENGTH=
MEAN RATIO OF LENGTH-DEVIATION TO LENGTH=
(.24
N= 26.
MEAN SIGNED DEVIATION OF DRIFT FROM CURRFNT MEAN (NEG=SLOW) -3.68
NUMBER CF DARK SPOTS=
3
NUMBER OF LIGHT -SPOTS=
23
DISTRIBUTION OF
)
TYPE
SN UMBER
0
OVAL
14
SLANT FESTOON
0
WAVE
2
ANGULAR
1
13.
N=
24.
SPOTS BY TYPE
AMORPHOUS
6
VARIABLE
2
PREC.
1
END
FOL.
0
END
_I~
SPOTS ROTATING
SLOWER
THAN CURRENT
MEAN LONG-TERM DEVIATIONS FROM MEAN DRIFTS=
1.99
N=
7.
MEAN SHORT-TERM DEVIATIONS (DEG.)
FROM MEAN POSITIONS=
*****
N=
MEAN OF DEFINITE OR PROBABLE LIFETIMES=
103.2 DAYS
N= 11.
MEAN PROPORTION=
2.0
N- 34.
6.5
N= 34.
MEAN LENGTH=
MEAN RATIO OF LENGTH-DEVIATION TO LENGTH=
0.22
N= 34.
MEAN SIGNED DEVIATION OF DRIFT FROM CURRFNT MEAN (NEG=SLOW) -8.72
NUMBER OF DARK SPOTS=
24
NUMBER OF LIGHT SPOTS=
16
DISTRIBUTION
19~
TYPE
NUMB ER
OVAL
14
SLANT FESTOON
0
WAVE
6
OF
ANGULAR
1
17.
N = 40.
SPOTS BY TYPE
AMORPHOUS
14
VARIABLE
0
PREC.
3
END
FOL.
2
END
r
SPOTS ROTATING
SIMILAR
TO CURRENT
MEAN
MEAN LONG-TERM DEVIATIONS FROM MEAN DRIFTS=
?.24
N= 15.
*****
N=
FROM MEAN POSITIONS=
MEAN SHORT-TERM DEVIATIONS (DEG.)
MEAN CF DEFINITE OR PROeA2LE LIFETIMFS=
80.5 DAYS
N= 10.
MEAN PROPORTION=
2.0
N= 41.
MEAN LFNGTH=
****
N= 41.
MEAN RATIO OF LENGTH-DEVIATION TO LENGTH=
0.23
N= 41.
-0.39
FROM
CURRFNT
MEAN
(NEG=SLOW)
MFAN SIGNED DEVIATION OF DRIFT
NUMBER CF DARK SPOTS=
25
NUMBER OF LIGHT SPOTS=
21
DISTRIBUTION
STYPE
NUMBER
OVAL
23
SLANT FESTOON
0
WAVE
7
OF
ANGULAR
0
22.
N= 46.
SPOTS BY TYPE
AMORPHOUS
11
VARIABLE
2
PREC.
2
END
FOL.
1
END
SPOTS ROTATING FASTFR THAN CURRENT
8.
N=
1.77
MEAN LONG-TERM DEVIATIONS FRnM MEAN DRIFTS=
*****
POSITIONS=
MEAN
FROM
(DEG.)
DEVIATIONS
SHORT-TERM
MEAN
7.
N=
170.9 DAYS
MEAN OF DEFINITE OR PROBABLE LIFFTIMES=
N= 24.
2.2
MEAN PROPORTION=
N= 74.
6.8
MEAN LENGTH=
N= 24.
0.21
MEAN RATIO OF LENGTH-CEVIAT ION TO LENGTH=
MEAN SIGNED DEVIATION OF DRIFT FROM CURRENT MEAN (NEG=SLOW)
18
NUMBER OF DARK SPOTS=
9
NUIBER CF LIGHT SPOTS=
DISTRIBUTION nF
t-
TYPE
NUMBER
OVAL
13
SLANT FESTOON
0
WAVE
5
ANGULAR
0
N=
13.59
20.
N= 27.
SPOTS BY TYPE
AMORPHOUS
7
VARIABLE
0
PREC.- END
FOL. END
,,~
'
APPITDIX D
Lifetime-size Relationships
128
~_C______
;
LIFETIME-LENGTH
LENGTH
WITHIN
LITFETIME
1 =
LIFETIMF
2 =
LIFETIME 3.=
LIFETIPE
2 DEGREES
OF
2
6
9.
17.
298.
RELATIONSHIP
10
40.
38.
160.
232.
14
18
22
26
46.
4 =
~a~~oc~ctspc
LIFET IME 5 =
52.
104.
180.
208.
6 =
24.
36.
29.
30.
L IFETIME
__
~rEc~ti~L~
71.
~iF~C~~t-rt~
I '
"-
I
~,rr
I
.hrrr. rna.rrl , u,,~nrr
~uu~-.
~,u~,,,,-p.l~m~.,x-~ua,~~-a,
r.-rr~-r
~l^-r-rr^,r^-r-l- ^_~I~
irsrr
iu~~-ar
LIFET IME-ARE A RELAT IONSHIP
AREA WITHIN 5
LIFETIME
SQ. DEG. OF
5
15
29
45
35
13.
L IFETIME 2 =
34.
40.
3.
LIFETIME 3.=
167.
190.
232.
198.
LIFET IME 6 =
26.
105.
35.
S~crb$
~a~dc~d~~
LIFETIME 4 =
5 =
65
f~Et~~F~
1 =
LIFETIME
55
sl~Saa~ $
46.
~et~Q~~Fs
OIsr4r~
Ir~prldc~Cr
1SC~CSICL
slr+lr
122.
208.
~FL~OI$~L
52.
49.
t~bc~rCr
trG~t
8
7t
i ' -.
~
,
4?
__
4
L
iP
C
_
_I_