MASSACHUSETTS INSTITUTE OF TECHNOLOGY
LINCOLN LABORATORY
MILLSTONE HILL THOMSON SCATTER RESULTS FOR 1969
Group 21
TECHNICAL REPORT 513
23 JULY 1974
Approved for public release; distribution unlimited.
LEXINGTON
MASSACHUSETTS/
/
I
AIR FORCE (1) APRIL 4, 1975--37:
AENTRACT
This reporf
summarizes
and ion tem~ratures,
the results
and vertical
ionization ff.xes
1969 using the Millstone Hill (42.6”N,
system.
These data,
gathered
over 24-bour observing
time resolution
fortheelectron-iensity
distribution,
fn the F-megion obtained during
71.5”W) Thomson (incoherent)
for the height interval approximately
pericds,
to obtain res”its
scatter radar
200 to900
km, were
ronghly twice percalendarmontb.
over this entire
45 minutes, depending uponwhicbof
electron
twooperating
The
height interval was either 300r
mcdes was employed.
The results for the diurnal variation of the electron density and temperature exhibit
the characteristic
tionbefween
summer
tbefwotakes
ral precipitation
and winter patterns discussed
place in April and October.
were observed
serve a stable red arc.
previously.
llvocases
ofoverheadauro-
during the year as a consequence
Other instances of geomagnetically
Thetransi-
of efforts to ob-
disturbed hehavior were
infrequent.
Vertical
fluxes of ionization
were measured,
and tbeflux
sphere near midday was found m have an avera~
Near midnight, the magnetosphere
escaping m the magneto-
value of -5
appears to s“pply thelocal
x 107 el/cm2/sec.
ionosphere witha flux
of about half this amount.
.
111
—
CONTEPiTS
Abstract
I.
11.
111
INTRODUCTION
EQUIPMENT,
PROCEQUR,RS
A,
Equipment
B.
Observing
C.
OBSERVING
A.
General
B.
Seasonal
6
,
Disturbed
Winter-NightB
38
Days
39
ehavior
Disturbed-Nighttime
ELECTRON-AND
41
Behavior
1ON-TEMPEUTURERESULTS
42
42
A.
General
B.
Quiet-Day
C.
Distm-bed-Day
D.
lon.Temperature
Electron
94
Temperatures
Electron
Ternperatm-es
~~~
95
95
IONIZATION.FLLK
RESULTS
95
General
95
B.
Steady -Stata-Velocity-
96
c.
Veloci.*.y Results
99
D.
Daytime
99
E.
Nighttime
F.
VI.
37
Variations
C.
VERTICAL
*i
RESULTS
11
D.
A.
,
3
Procedure
Data Reduction
E.
v.
2
2
111. ELECTRON-DENSITY
IV.
AND DATA -PROCZSSI?IG
vs-He.igk,t
Flux Results
f~i
Flux Results
Flux Through
Profi!es
147
65o km
130
SUMMARY
APPENDIX
136
References
iv
.
MILLSTONE
HILL
THOMSON
SCATTER
RESULTS
FOR
1969
INTRODUCTION
I.
Since
3963,
densities,
Massachusetts
presents
ported
incoherent
andelectron
(42.60N,
the results
were
in earlier
made
years
to the World
(Thomson)
7i.5sW).i-6
radar
measurements
have been
measured
This paper
is the seventh
gathered
inthisprogram
during
for periods
of 24 hours,
approximately
have been published
mta
scatter
and ion temperatures
Center
A,
in the articles
Boulder,
in a series
calendar
listed
of F-region
at Millstone
year
twicea
West ford,
of annual reports,
1969.
month.
in Table
electron
Hill,
and
TheobservationsreThe results
obtained
I, and have been transmitted
Colorado.
TABLE I
PUBLICATIONS
CONCERNING
THE MILLSTONE
HILL UHF
(68cm Wavelength)
THOMSON
SCATTER RESULTS
Year
Publication
Months Covered
February
1963
March,
1963 to Jonuary
July,
April,
July,
January
August,
Ref. 1
1964
September
Ref. 7
November
thro.gh
Ref. 8
Ref.2
December
1964
April,
July,
January
Jonuary,
November
Ref. 9
through December
April,
Ref. 3
Ref. 10
August
1965
Ref. 11
June
June,
August,
January
Ref. 12
September
through December
Ref. 4
I 966
January,
January
March,
July,
September
Ref. 13
through December
Ref. 5
1967
February,
January
June,
October,
December
Ref. 13
through December
Ref. 6
1968
0ctc6er
During
i968
a component
by electrostatic
gatheredbys
reported
waves
inthe
tudent~~:6mthe
elsewhere.
In addition
tically
and 1969,
of the reflected
directed
Ref. )4
the UHF Incoherent
signals
electron
scatter
radar
system
known as the “plasma-line.tn
gas impressed
University
of lUinois
was also
These
employed
reflections
by fast photoelectrons.
and the University
These
of Michigan,
to study
are produced
results
were
and have been
,
to the measurements
UHF radar
system,
reported
a number
here
of F-region
of measurements
observations
were
made with the ver -
conducted
in i969
of the
E-,
and F2 -regions
Pi-,
measurements
horizontal
were
During
required
pointing
a solution
height range,5
were
could
from
of the ground-clutter
A digital
sweep,
employed
studies
dwing
i 969.
shift
A.
of pairs
function.
and no fm.ther
the
heights.
This
observations
achievable.
of short
o“t any echoes
These
little from
Sections
temperatures,
in this
Both require
pulses
whose
that appearad
However,
-
spacing
to be co-
this system
discussion
of it will be pre-
observing
those
employed
111through
in the latter
V present
and vertical
a calculation
and data-processing
ionization
is presented
part of i96i2,
the results
fluxes,
procedures
and
of the synoptic
while Sec. VI pro-
of the magnitude
of tbe unwanted
by tbe transmitter.
0BSERV2NG
AND
DATA-PROCESSING
PROCEDURES
Equipment
Tbe UHF incoherent
interfaced
analyzer
directly
but require
comment
hi the new spectrum
In addition,
scatter
portion
radar
equipment
of the receiver
the signals
described
These
previously.4
by one of newer
changes
During
design
4968,
that was
are fully docmnented
in Ref. 20,
here.
analyzer,
thereby
the integration
eliminating
are no longer
to a bank of 5 -pole
has been
was replaced
into the SDS 9300 computer.
further
SDS 9300 computer,
ployed
of the equipment,
In the Appendix,
introdwed
the spectrum
crystal
of the echoes
virtually
gated from
filters
all problems
the time base,
each of which
is carried
out digitally
due to gain differences
but instead
is matched
by the
and drift.
are continuously
to the length of the pdse
ELp
em-
(0.5 or f.O msec).
Each of the (two) filter
frequency
pled sequentially
manner
the impulse
returned
i 969 the 0.5 -msec
quency
commutation
a dmble- sided
gathered
compensation
after
of several
to tbe manufacturer
filter
employed
was still
delay
the outputs
the 0.5 -nmec
outputs
are sampled
Since
line is used
between
correspond
matched
*Ii. 5 kHz about the radar
for repair,
to drive
samples,
were
to position
obtained;
Nm.ember
with only half the filters
the filters,
however,
psr unit time.
2
in a
although
real
it
altitude.
in service
(in
Accordingly,
1968 aud February
in place.
with respect
the filters
placed
inter-
must be sam-
Thus,
to the same
filters
and between
at 0.5 -msec
tbe filters
of them was fcund to have deteriorated.
bank was operated
scheme
spectmm
spanning
75 km of altitude.
for the delays
all filters,
a few months
response
24 filters
at the filter
every
of 20 psec ), a tapped
to scan through
Unfort””ately,
were
exact
employs
The voltages
may be obtained
(at intervals
that provides
480 psec
4968),
banks available
with i -kHz spacing.
so that a spectrum
these
the height resolution
consisting
until 1970,
of operating
prevented
was used to subtract
form
a summary
densities,
EQUIPMENT,
takes
that previously
tbe echo autocorrelation
differed
620
been documented.
,
of F-region
doppler
vals
computer
and to compute
lf provides
a summary.
plied
of improving
transmissions
into final operating
have previously
11.
problem
a new method
to E- and Fi -region
here.
Section
vides
work began m developing
to extend the measurements
as well as a means
was not brougbt
sented
of +969,
radar
met by employing
be varied.
herent
radar with the beam directed obliquely.
These
47,18
and the
the ion composition
in the FI -region,
i4, i9
Inasmuch as these results have also been reported,
in this paper.
the last quarter
UHF vertically
f
the L-band
at determining
drift in the E- and F-regions.
they are not included
ments
employing
aimed
Owing to the fre-
to the signal
only half as many echo samples
spectrum,
were
.
.,
No further
difficulties
a dism.epancy
between
pulses
persisted.
height
interval
agreement
using
the 0.5 -msec
moved
it appears
the observations
exactly
i.0
msec
application
Of the
SigKMIS
of the first
sample,
4970,
pulses,
were
filters
prior
to the filter
source
cause
of error
samples
although
and 1.0 -msec
over
lengths.
the
The dis -
of the ion temperature
of this difficulty
pulses,
existed
pulses,
is believed
to be
and an empirical
which compounded
the receiver
being taken from
bank produced
the i.O -msec
the time when the suppremion
estimates
to the transmitted
with i.0 -msec
to the first
thus rendering
with 0.5-
was observable
made with both pulse
by lower
1969,
(see below).
that a second
conducted
during
obtained
in Ref. 20,
The principal
devised
analyzer
temperature
measurements
by the 0.5 -msec
was eventually
In retrospect,
For
for the plasma
at night when it was manifest
provided
s cbeme
with the spectrum
which has been discussed
450 to 750 km where
match
correction
lem.
the results
This error,
was largest
Ti observed
the poor
were encountered
transients
results
is removed
suppression
the filter
this probwas.. re The sudden
bank.
which had not died out by the time
at 450 km slightly
was advanced
in error.
hy 0.5 msec,
In October
thereby
diminishing
this effect.
The most
of antenna
surface
serious
following
gain
Gain measurements
encountered
a snow storm
of tbe antenna iced
was - i2 dB.
over,
the course
late in February.
to within 2 dB of its earlier
the mesh
produced
value.
by tbe snow load.
through
the radio
being
loss
1*worked!,
the gain was found to be i.4 dB below
tolerance
was measured
design
value.
the surface
in a survey,
A repetition
of these
was retensioned
laid diagonally
across
In December
events
unwanted
ground-clutter
echoes,
horn feed
that increased
the directivity
over
the power
feed support
structure.
efficiency.
from
B.
Observing
During
Table
1969,
II lists
duced;
to detect
were
repeated
urement
we attempted
to
value.
i.e.,
and during
surface
to the original
the mmmer
by means
to
by the end
when the rms
close
of
returned
Thus,
2n June,
of that yea?
of a set of cables
to the antenna,
was the addition
The taper
and,
more
a quarter-wave
appears
the effective
to the conical
collecting
off the tripod
which raised
to broaden
of
This had the ef-
importantly,
choke,
to have been
to reduce
of the intensity
about 40 to about 20 dB.
edges
altering
designed
of an extension
feed pattern.
from
incorporated
to make observations
for which
is the mean of tiie planetary
the introduction
were
by the distortion
as the surface
gain
and the gain
the horn
the beamwidth
area.
Procedure
the vertical
servations
This
off the reflector
significantly
the dates and times
included
Following
mesh
in antenna
by hand,
was caused
strength
of modifications
of this modification
about 0.7- to O.8“ without
that the loss
of the temperature.
in 1970,
of the primary
~he extension
The net effect
loss
its previous
was increased
scattered
the i -inch
loss
structure.
was made.
the reflector
showed
decreased
cycling
occurred
the pipe supporttig
the illumination
residual
with additional
%969, the last of a series
fect of reducing
this storm,
it was found to be 1.05 inches,
and provided
i 969 was a dramatic
the snow was removed
gradually
by daily
of April,
During
star Cygnus
This
This
during
with snow to a depth of 22 feet near the center.
of the next few days,
returned
shape
with the equipment
and the dish filled
made by observing
During
its original
)
difficulty
drift
conducted
four times
45 minutes.
magnetic
of the new spectrum
of the ionization
in which
twice
measurements
above
per month for periods
were
successfully
index Kp over
analyzer
in i968,
hmax l?2 (Ref. 20).
each period
special
of 24 hours.
carried
of observation.
efforts
For this reason,
the measurements
made using the 1 -msec
6,2o
in each cycle.
This raised the time to complete
out and re -
were
some
made
ob-
pulses
( vC -moden
a cycle
of mess-
)
.
TABLE II
lNCOHERENT
Begin
5CATTER
051 SERVAT10NS
End
Date
c’
EST
Date
16 J.wary
0930
17 January
30 January
2000
31 January
5 February
0930
6 February
12 February
0520
13 February
26 February
1030
27 February
21 March
1620
22 March
23 March
2040
24 March
25 March
1630
26 March
9 Apri I
0930
10 April
2220
24 April
0800
7 May
23 April
6 May
‘q
30 May
OBOO
– 1969
Mean
c*
EST
D
D
D
Q
Q
31 May
Kp
C4st
0930
3-
Reg
0800
10
Drift
0900
3-
Reg
0950
2+
Drift
1030
30
Reg
0510
w
Reg
0500
70
Reg
1630
3+
Drift
0930
2
Reg
2210
2-
Drift
OBOO
2-
Reg
0130
2+
Drift
0630
1+
Drift
0900
l–
Reg
OB1O
20
Drift
0
COmrnents
Incomplete
Antenna
gain dwm
10 dl
SpecirA OUrwel opemfim
Quiet
Combined
I June
5 June
q
2030
2 June
0930
6 June
Q
?3 June
QO
B20
24 June
I July
DO
800
2 July
0815
3–
Reg
0540
10 July
0440
2-
Driff
800
3 0 July
I 900
20
Drift
9 July
!9 July
Ql
!4 August
!6 August
D
Quiet
o815
I 5 August
q
o845
1-
Reg
1530
2 7 August
D
1530
3+
Drift
o900
2
Reg
o800
2+
Drift
900
50
Reg
Speciol
700
10
Drift
Q.i.t
I 700
20
Reg
Drift
Reg
9 September
o 915
I O September
!3 September
oBOO
2 4 September
9 September
D
22 00
1 Octcber
4 October
Q
1700
I 5 Octcber
3 November
D
14 00
O November
q
8 December
I
DO
QI
4 November
0
08 30
2 1 November
Q
1Ooo
1-
124s
9 December
D
1245
2+
Quiet
oumxal operation
Quiet
Ccmditi.n:
Q
q
D
One of five quietest days i“ nvmth
One of ten quietest days i“ month
0“.
of Five most distutbed days i. month
Obserwticms:
Dat~ gathered
and anolyzed
m described
Reg = Regular;
Drift = Drift
Measurement.
;. Li”c.al.
4
I.cibora<ory Technical
Report 477 (Ref. 20).
,
.
In the normal
pulses
operating
in sequence,
mode,
the complete
measurements
cycle
in Table
II to distinguish
24 hours
of each type of measurement
The value
of the F-region
measurement
which stored
ment,
those
frequent
with all the other
ionosonde
was modified
well as to have its frequency
would turn on tbe sounder
turn was just perceived
carried
controlled
by a remote
the frequency
range.
on magnetic
tape.
into the computer
To make the measure-
synthesizer.
of the synthesizer
dials
of a
of each cycle.*
on and monitored
frequency
The synthesizer
in the form
at the start
who then typed tbe value
it to be turned
‘Tregular”
Usually,
month.
wai? made available
in megahertz
information,
and %.0 -msec
of ‘! drift:f
out in each calendar
operator,
to permit
0.5-,
runs are termed
the determination
y foF2
and advance
at great
These
in the data reduction
critical
was made by the radar
it, along
the C-4
made using 0.4-,
30 minutes.
emphasizing
were
of Nmax to be employed
measurement
This
them from
were
occupying
remotely,
Thus,
as
the opew.tor
until the F2 ordinary
then gave the required
re -
value of
foFZ.
The intent of this procedure
quired
for processing,
However,
the radar
night.
Thus,
stead,
they were
and values
operators
as a rule,
these
plotted
recorded
West Virginia.
lowed
the variation
onto IBM cards.
encountered
estimates
cm’ve
at Millstone,
were
together
Maynard,
this curve
from
espectilly
at variance
in-
and Wallops
of points
Is-
that fol-
with the observations
at 30-minute
between
at
the film records
(if available);
this collection
employing
interpolation
foF2,
re-
of a run.
in the data analysis;
derived
Massachusetts
then processed
by linear
in reading
with those
when this was clearly
read from
data were
obtained
difficulty
all the information
upon completion
were not employed
was then drawn through
except
Values
profiles
of time,
Canada;
A smooth
The recorded
electron-density
out immediately
frequently
as a function
stations.
a data tape that contained
be carried
real-time
at Ottawa,
land,
at all the other
was to create
so that this could
intervals
values
and punched
of Nmax for the
the values
avaflable
at half-hour
internals.
During
4969,
Dr. J. Noxon
other
the first
(Harvard
emission
from
objective
arcs
observe
of low-latitude
d.
auroral
activity,
Unfortunately,
twilight,
and it requires
notification
of people
3n the past,
scatter
were
i
approximately
at their homes,
although
some
Alouette
1.
optical
with measurements
coincidences
observations
* Nmax: = 1.24 X i04(foF2)2
el/cm3
red-arc,
for the activity
way.
due to the high
gathered
at Millstone
to have declined
This appears
SAR-
us to tbe presence
is not detectable
operations
and
and deter-
as no overhead
were
luminosity
6300 -~,
Massachusetts.
excitation
results
with
simulta until after
fo220wing
substan-
to have been the case
4969.
gathered
between
were
auroral
II) Dr. Noxon alerted
to commence
were under
Boston,
of impact
and radar
it was POSsible
the 5577 -~,
to be disappointing,
(Table
have been made to compare
on lucky
early
proved
two hours
measurements
on 29 September
efforts
obsermtions
dependent
and valuable
a stable
for in terms
on two occasion8
measurements
Observatory,
owing to tbe fact that the auroral
by the time the radar
for the measurements
was to observe
be accounted
coordinated
was measuring
at the Blue Hills
fn this the effort
However,
neously.
tially
could
made to conduct
at that time,
of this joint effort
of the electrons.
were
who,
the night sky,
mine if the 6300 -~ emission
temperature
were
University)
lines
The principal
attempts
by various
our operations
schedule
when foF2
the observations
d to coincide
is expressed
1
5
gathered
,satellites.
and satellite
with passes
in megahertz.
in the incoherent
Usually,
passes
the comparisons
over
of the topside
Millstone,
sounder,
.
Beginning
Alouette
in i 968,
a number
11 at the request
observations
also
satellites.
were
Where
favorable
passes,
operations
of scientists
possible,
the regular
111lists
scheduled
short
ohserving
periods
purpose
measurements,
C.
in July t 968,
of interest
The computer
were
programs
spm-ious
of Te/Ti,
plotter,
employed
echoes
Debye
were
as functions
The values
with
2 hours)
for these
cm request.
of OGO VI was to permit
~id & &u
probe
Comparisons
spectra,
with
Unfortunately,
At high altitudes,
comes
inaccurate
better
pulse
value to yield
tbe absolute
the dependence
the correct
on altitude
as a graph plotted
prolengths.
varia-
by a Calcornp
Estimates
of Te and Ti were also
corrected
for the effects
provided
of the changing
in which the measurements
were
of Te and Ti were
obtained
by extracting
width (proportional
freqwmcy
(proportional
thathad been obtained
expressions
scaling
theoretical
power
length is extremely
of the transmitter
pulse
two parameters
to Te),
and the ratio
to Te/Ti).
to represent
spectra
small.
These
Te and Ti,
computed
In computing
and the finite
assuming
these
the-
width of tbe filters
in
.
in the &bye
(
length
temperature
T
obtained in the above manner for
‘ohs
20
on the spectrum,
use was made of the expression
1.62 x Te
-i
ob s
i–
N,
holds
(1)
)
only so long as the second
term
in the parentheses
remains
T
may be of the order of 2000 to 3000 K and the ~o=rection
then ~‘ohs
as Ne approaches
i 04 el/cm3.
Tbw,
the electron
temperatures
obtained near
this level
The existence
the electron-density
i963.
of the electron
this expression
<0.3.
possible.
were included.
the estimate
of tbe change
all the
became
made with the three
the manner
to that at the center
the effects
the measurement
together
reduction
Basically,
was avai3able
20
that placed
machine
(4) removed
profile
and that the Debye
‘ohs
are believed
of an em-or
response
to be overestimates.
in the 0.5-rnsec
of the i.0 -msec
(B-mode)
pulses
6
!
Results
I
in routine
(typically
IV.
sounding
in a manner
(3) adjwted
of Te were
and width through
T==T
obviously
to coincide
that occurred
have been reported.
in Ref. 20.
the half -peak-power
into analytical
of the ratio
To correct
or above
the passes
measurements
V contrasts
since
viz.,
in the wings
inserted
ore tical power
the effect
Table
spectra,
only 0+ ions are present
distorting
This
be noted that the estimates
of the peak power
values
are described
as log, o Ne vs altitude.
in each year
the measured
gathered
on the ionosonde,
and on the printout.
It should
were
due to satellites,
length with altitude.20
made and reduced
from
in Table
by remote
i 969,
I, 11 or ISfS I have yet to be made.
(1) combined
and on Debye length.
and on a printout
on plots
during
data tape so that complete
in a way that:
value of Nmax F2 as measured
tions
During
but may be made available
of this exercise
in Alouette
the results
on a single
obtained
(2) removed
made
scheduled
of operation
as listed
deduced
Center.
of
ISfS I, OGO VI and Alouette
of MiUstone
periods
with passes
Reduction
Beginning
files
of the results
sounders
short
in this report,
of the measurements
and most
were
overflights
passes
Flight
(AE-B),
operations
Additional
satellite
and ion temperatures
of the topside
Data
quantities
with other
are not included
of electron
the records
monttly
to coincide
Space
of the Explorer
the satellite
with this in mind.
to coincide
The primary
passes
and Table
scheduled
we=e scheduled
at the NASA Goddard
made during
were
comparisons
of observations
=esults
to an applied
has been noted.
RF pulse,
Owing to the
it was assumed
that
TABLE Ill
SATELLITE
PASSES DURING
Date
REGULAR
OPERATIONS
Height
(km)
Time
(SST)
IN
1969
Satellite
25 March
2041
910
10 April
0537
30May
1904
650
1200
23 June
I743
OGo
VI
24 June
0407
OGO
VI
I July
1647
OGO
VI
2 July
0312
OGo
VI
9 July
1550
OGO
VI
10 July
0215
OGO
VI
23 September
1725
630
[s1s I
29 September
2149
974
Alouette
I
30 September
2202
942
Alo.ette
I
Alouette II
1s1sI
AE-B
TABLE IV
SPECIAL
OPERATIONS
COINCIDING
WITH
SATELLITE
PASSES IN
Time
(EST)
Height
5 May
1541
584
Alouette
IB June
1800
640
OGO
VI
19 June
0420
430
OGO
VI
27 June
1626
OGO
VI
Date
(km)
1969
Satellite
I
0849
650
1s1sI
29 SepterAber
1725
587
1s1sI
I 7 Octcber
1453
730
Isis
17 Ockber
1937
625
Alouette
20 Octcber
153a
785
1s1sI
27 Octcber
1945
513
Afwette
II
29 Octcber
1809
512
Alwette
II
4 August
.
I
11
TABLE V
OBSERVING
Length of
Each Cbserving
Pericd
(hours)
Year
AS A FUNCTION
Time Taken
tO Mewure
Number of
Observing Periods
per Mcmth
One Profile
(ho”m)
4
1.5
30
1963
PROGRAM
OF YEAR
Number
Profiles
of
Reduction
Chined
Methcd
Employed
per Month
80
Mean
hourly profiles
constructed
calendar
(Ref. 1)
1964
30
2
1965
48
I
1966
24
2
1.0
0.5
0.5
60
Asin
1963
96
Asin
1963
96
Each prcfile
analyzed
separately
1967
24
2
1968
24
2
0.5
0.5
96
or 0.75
Asin
96 or 64
for each
mdnth
(Ref.4)
1966
Asin 1965 until J”ly
when ccmplete
nwchine
~
I
reduction
began (Ref. 20)
1969
24
0.5or
2
0.75
96 Or 64
Machine
reduction
(Ref.20)
the error
stemmed
0.5-msec
pulses.
from
Ln order
response
for the B-mode
the same
height.
sistent
results
possible
This work was carried
results
obtained
were also
ratios
linear
version
below
because
were
in error)
well matched
made to determine
spectra
Lejeune .*
number
obtained
the proper
Ln part,
were
of points
4.4 “sing
in Figs.
of the analysis
the Centre
ratios
in this figure
the shorter
pulses.
reliable
It seems
was made at 450 km (where
because
theerror?.ppew-s
suggests
corrections
by the two different
of
as a func-
-mode
results
that (Te/Ti)C-mode
are applied
to B-mode
pulses
des Telecommunications,
8
to de.
values
that it is difficdt
for the B-mode
they assume
program,
i
at
and con-
compared.
A plot of ( Te/Ti)c
measured
Nat,{onal d! Etudes
spectrum
to
vs Ti
a bias of up to 200 K can be seen at low values
that have been devised
1 and 2, i.e.,
to
in the two modes
Unfortunately,
of spectra
the comparison
and,
to be less
correction
corrections
curves
if the temperature
,>011 leave from
Seine, France.
in part,
is shown in Fig. 2, where
The empirical
in a later
heights
out byG.
The distribution
– Ti (C-mode)
on the smooth
appeared
by comparing
a large
somewhat
filters
was obtained by J, E. Salah by comparing
22
at 525 km with the two pulse lengths.
Fi&Vre ~ shows (Te/Ti)B-mode
temperature
of Te/TT
efforts
although
failed,
An empirical
tion of (Te/Ti)C-mode.
resolve
this,
empirically
were not obtained,
penal upon Te/T<
(B-mode)
to remedy
fHters
that this approach
the i-msec
Te/Ti
the fact that the B-mode
are based
is COITeCt.
results
at 525 km differ
Issy-les
at aLL
by more
- Moulineaux,
.
than 0. i,
These
or if the ion temperatures
corrections
derived
from
the two pulses
differ
i < Te/Ti<
i.47
by more
than iOO K.
are:
0.425 (Te/Ti)
(Te/Ti)’
❑
(Te/Ti)t
= i.5(Te/Ti)
( Te/Ti)
+ 0.575
– i
‘ = Te/T,i
1.474
Te/Ti<
Te/Ti
>2
(3)
2
(4)
1< (Te/Ti)l
T; = Ti + ZOO
(2)
(5)
< i.2
T; = Ti - 333( Te/Ti)’
+ 600
i.2<
(Te/Ti)l
< i.5
~ (6)
T; = Ti – 200( Te/Ti)’
+ 400
1.5<
(Te/Ti)l
<2.25
(7)
<3
(8)
T;=
T;
❑
Ti–50
2.25<
(Te/Ti)l
T.
1
(Te/Ti)l
(9)
>3
(40)
T~ = T~(Te/Ti)’
where
original
the primed
quantities
measured
values.
are the comec ted parameters,
‘..
\
and the unprimed
quantities
are the
o
“0limca
0
28 —
2.6 —
.0
❑
0.
2.4 —
o
,.2 —
o
g
t
n
.s
2.0 —
~.
.
O.
,.s —
.“
n
525 km
,.4 —.
.
.
14-!8
●
8-7
o
,7-,8
❑
28-2,
AUO 69
JAN 70
AUG 70
DEC 70
,,2 —
!.0
!.2
14
!.6
,,
,,
22
2+
“
“
3
[T. (T,lC
Fig. 1.
Te/Ti
derived
from 0.5-msec
(B-mode) and 1. O-tnsec (C-mode)
22
pulses.
3.0
[48-2 -!0442.!
I
❑
,. e —
I
,.6 —
,8
“
m,.
e.4 —
❑
,2
—
.
“o
o
~
■
~- 2.0 —
~.
■
!,8 —
o
!.. —
.“
525 R.
.
,4-15AuG
0
17-18
❑
28-29
.
,.4 —
69
AUG70
,.2 —
I
I
,.0
-20.
-,00
0
(00
TEMPERATURE
T,wll-rl
Fig. 2,
Dew iaticm between
(C-mode)
Since,
report
were
C-mode
only
examined,
the uncorrected
the influence
by constructing
(i-IIISeC
of Ne,
tion of these quantities
Te,
As described
over
and a simpler
limitations
program
that reduces
spectra
were
B-mode
results
senting
these
does
include
using O. 5-msec
range
earlier.4
(B-mode) and 1. O-msec
doppler
B-mode
at the time the data in this
results
profiles
(chiefly
at night in summer)
that largely
depended
on the
tbmgh
and time.
shift,
program,
to obtain drift
less
for F-region
these
vertical
diagrams
showing
to extract
of drift velocity.
gave almost
method
the variaThese
were
identical
Later
was modified
the program
has been devised,
To date,
obtained
from
Owing
only the C -mode
to include
no method
owing to their
on request.
these drift
results.
op-
in the main
Initially,
to be valuable.
the signal
The theoretically
was incorporated
data can be made available
fluxes
from
and temperatures.
proved
form
developed
17method
this latter
estimates.
graphical
However,
were
and hence
densities
accurate,
contour
.
‘1least -mean -sqwres
data in a convenient
results
available
150 to 900 km (200 to 900 km at night).
of methods
the data to obtsin
which,
were
-vs-height
outlined
in the analysis
analyzed
both with height
of the poor
the height
of the overall
to space
results
temperature
in Ref. 20, a mmber
estimates
method
derived
and Ti were used to construct
drawn by hand in the reamer
timum
(°K)
[c]
data.
pulse)
The profiles
spectra
Lx temperature
200
pulses.22
however,
was minimized
DEC 70
the
of pre -
wide spread
This
measurements
report
(Sec. V).
io
..-...—...
——..
——
111. ELECTRON-DENSITY
A.
General
Contours
Figs.
of the logarithm
3(a) through
which logio
4.0 (e. g.,
were
tithe
May were
made
(z).
Ne > 3.2.
of the equipment,
30-34
RESULTS
(logio
The contours
It is possible,
valley
some
marred
on 1-2 June.
that forms
however,
between
days (e. g.,
by a failure
These
Ne) of the electron
are drawnat
30-31
tithe
two sets
density
intervals
that the results
the E-and
January)
Ne (el/cm3)
of 0.2 over
F-layers
become
analyzer,
unreliable
at night).
are incomplete.
spectrum
are presented~
the range
when logio
for
Ne<
Owing to malfunctions
The observations
and additional
of data have been combined
of altitudes
for
measurements
into a single
conkmrp lot
[Fig. 3(l)].
.
[.1
Fig.3 (a-z).
C.ntcwrsoflog,
oNe .bserved
if
on days listed in Table
Il.
w
3.4
7m@L
3,4
-
.OO,O N,
,0-3,
,,.
4%,
4.6
7C0 —
60. —
m.
.CO
\Y4’”
—
,?
X/
b_’Q...-..J2
BJ3
,0
—=---=Qo
.“,,.
I
1
I
,m
,2
58
/
6.0
,.-
-
,--—-_—
~___
------
---
.,
.-.
5.0
/’
::
.-.’
%8
,.6
~’”
$i
ES,
[b)
.
Fig.3 (a-z).
Continued.
,,.
[<)
Fig.3 (a-2).
Continued.
.
EST
(d)
Fig.3 (a-z).
Continued.
Ez!!L
:
:
r,
r
50
::
44
..2
4,0
,0
3.6
3.4
3,2
EST
(d
Fig.3 (a-z).
Continued.
i5
.
(f)
~9.3(a-z).
Continued.
46
,,. .. ”....,
7.,
40!
>0
tm.
u...
.0..
,*T
(Q)
Fig.3(o-z).
Continued.
.. ..
—
m
/.. ----
-.
q
::;
F*
h. . .
J
.,
‘----
,.-”
5.6
5.4
/
3.4
3,2
4.0
R
(h)
.
Fig.3 (a-z).
i8
Continued.
.
,qg.3 (0-z).
Continued.
I
i9
Fig.3(a-z).
Continued.
20
[k]
Fig.3(a-z).
Conti..ed.
(1)
Fig.3 (a-z).
22
Continued.
3.,
s.8
“F
4
@%Na
5-6
‘UN 1969
4.0
am
44
,.0
4.,
r---’
4,
:;
4.0
3,
::
3.2
,
,,..
>
,m
,
lam
EST
[.1
Fig.3(.-z).
Continued.
23
w
IW~
zoco
zzou
*“W
1
lEim
“-’’J+--’
m. –
‘%
/
N. 23-24
JUNN,,
5.2
:
:
g ,@
I
mu
L
E,,
(n)
.
Fig.3 (a-.).
24
Continued.
—-
lmE!zL
,..
.~,
3.8
F
N,
l-t
4.4
4,0
m.
4.2
,..
{
4.6
Y-
1
(.)
Fig.3 (a-z).
Continued.
25
WL
(969
.
Fig.3(a-z).
&nfinued.
26
L
,00
h
//1
/
.00
:
>
‘2
,.0
:
4.0
,..
,.0
4.8
4.6
+4
4.2
4.0
38
36
,.4
3.2
2..
EST
(,1
Fig.3
(a-z).
Continued.
27
EST
(r)
Fig.3 (a-z).
28
Cmjtin.ed.
[*1
.
Fig.3 (c-z).
Continued.
29
Fig.3 (a-z).
30
C.antinued.
(U1
Fig.3 (a-z).
Continued.
34
Tmm_
,..,...
,0.
-—
,.-,50,7
Lb-----i
3.6
,969
J/_ld
\
(w)
.
Eg. w-z).
Continued.
TmEiL
\
Ku /---.?8
,/
‘\\
/’l
/
,0, –
/
/’
----,4,0
_..-.
:
/‘
<
:. >0.
w
,Scc
,Ccm
am
,,m
EST
[“)
“
fig. 3(a-z).
continued.
34
mmEL
:
:
q
5.2
50
4,,
4.6
.,4
4.2
4.0
3.8
3.,
3.4
3.2
4,,
4,,
4.4
j:~
3.6
EST
[Y)
.
Fig.3 (a-z).
Continued.
35
(21
Fig. 3(CI-Z).
,—
.
Continued.
. . ..
B.
,.. ,..,
Seasonal
Variations
As noted in earlier
two characters
principal
tic patterns
features
i -6
reports,
There
(2)
The highest
(3)
FoJ20wing
variation
that we have termed
of the winter
(i)
the diurnal
is a large
behavior
dim-ml
values
of the electron
IIwinter!!
and !rsummer,f
follows
one of
respectively.
The
are:
variation
(e. g.,
5: i ) in peak electron
of Nmax are encountered
sunrise,
density
the electron
density
near
rises
density
i 300 local
Nmax.
time.
to its peak near
i300
and then falls
again smoothly.
(4)
The peak height hmu
above
(5)
lies
in the range
density
decays
250
km by day and rises
to 275
to
300 km at night.
At night,
pears
(6)
usually
the electron
to be maintained
on many occasions,
associated
i.mmedia tely after
for the rest
there
to a value
in Nmu.
This
that ap-
of the night.
is a post-midnight
with a downward
sunset
motion
increase
of the layer
and a lowering
is usually
of the plasma
temperature.
Figures
For
3(a),
(b),
(w),
the observations
mer behavior
havior
between
by i4-i5
(2)
There
here,
March
representative
there appears
and 9-{0
April
[Figs.
may be characterized
is only a small
highest
Following
changes
(4)
of the winter-type
from
variation.
winter
3(h) and 3(i)] and a return
to sum-
to winter
be-
value
diurnal
as follows:
variation
of Nmax is usually
in Nmu
sunrise,
little
the electron
throughout
The peak height usually
less
density
the rest
(e.g.,
encountered
2000 hours ), and is then considerably
(3)
examples
to have been a transition
[Fig. 3(w)].
bebavior
T&
and (z) provide
25-26
October
The summer
(i)
(y),
reported
< 2:i).
near ground
than encountered
increases
sunset
in winter
(e. g.,
i 800 to
near noon.
for only i to 2 hours,
and then
of the dayt tie.
lies between
275 and 300 km by day,
i.e.,
higher
than found
in winter.
(5)
The thickness
of tbe F-layer
is considerably
Figures
larger
(6)
At night,
tbe density
3(j),
(k),
(n),
(m),
(P),
(e. g.,
in summer
decays
(q),
as measured
between
points
of half-peak
density~
than in winter.
continuously
until sunrise.
(t), and (u) appear
to be representative
examPles
of this
type of bebavior.
The transition
pletely
of this change
These
from
summer
new state for the upper
winds
thereby
sponsible
is a seasonal
serve
altering
variation
to transport
the ratio
for removing
made that are consistent
to winter
atmosphere.
bebavior
is fairly
There
now appears
in the neutral
atomic
oxygen
of the ionizable
from
constituent
rapid,
and appears
general
wind pattern
of tbe upper
the summer
to the winter
(0) tO the mO~ecu~r
to signal
a com-
agreement
that the cause
io-13
atmosphere.
hemisphere,
sPecies
(02. N2 ) re-
satellite
observations
of neutral abundances have heen
23,24
measurements
of the wind system responsible
with this hypothesis,
0+ ions.
have not been made in sufficient
While
detail
to confirm
37
their
role.
It is also possible
that there are
seasonal
variations
However,
aPPear
in N2 and/or
measurements
made
Disturbed
have described
4-6,11-44
storms.
magnetic
and 29 September,
i.e.,
observations
subsided.
Ouring
variation
the 23-24
at heights
of N2 in the lower
in these quiet -day patterns
magnetic
storms
behavior.
near
thermmphere.
the S. C.,
period,
two of these.
(S. C. ) at about 1300 EST on 23 March,
a“d were
March
(Table
began
which promptly
at Millstone
II), hy which time the storm
of foF2
at
Addi-
largely
had
with the behavior
were obtained
and we were
scatter
i4 lblay,
[ Fig. 3(h)].
readings
in the D-1ayer,
during
echoes
obliged
on the ionosonde
to reconstruct
in the manner
outlined
the time
in Ref. 5.
the results.
TiEEmL
.
MILLSTONE
10NOSONDE
-OBSERVER
ESTIMATE
x
MILLSTONE
.
wALLOPS
o
ESTIMATE
OASED
ECHO INTENSITY
IO NOSONDE -FILM
ISLAND
ON INCOHERENT
SCATTER
..
.
Fig. 4. Variaticm
fcm 23-24 March
0
incoherent
of fOF2 MHz obtoined
1969 from v.ari atim of
scatter
power
during
period
when i.mosonde was at tiines blacked
out.
xx
.
0
i
I
I
,800
I
I
20,0
I
“q
I
I
2400
,,,,
I
I
moo
I
I
0.00
EST
As can be seen
and height.
with altitude.
located
curring
there
appeared
of ground
of -105
temperatures
at the time.
were large
much higher
While the interpretation
in the E-?egion,
with a density
electron
in Fig. 3(g),
The F-layer
hy the presence
reflections,
of the results
and that the “alley
el/cm3.
We believe
observed,
More
detailed
-
changes
in layer
than normal,
it appears
obtained
that there
between
calculations
shape
below
performed
only S1OW1Y
maximum
of ionization
was filled
with ionization
taken together
of soft (>400 eV)
varied
i7 O km altitude is complicated
the E- and F-layers
are being
as well as peak density
and the density
was a second
that this behavior,
is a manifestation
38
,,
25
i tO km
25,26
The March
until 0500 EST next morning.
[ Fig. 3(g)] may be contrasted
few reliable
of the incoherent
Observations
continued
observations
absorption
mcountered
in $969 on 24 March,
data during
5+ for the next 39 hours.
March
the intensity
occurred
enough to gather
[ Fig. 3 (f)] and a day later
the disturbed
of increased
from
major
made on 25-26
the storm
4 presents
changes
variations
commencement
after
were
Thus,
as a result
Figure
Three
exceeding
7 hours
two days before
seasonal
and we were fortunate
to Kp valws
2040 EST,
in F-region
and at Mills tone of N2 densities
Of large
previously
began with a sudden
gave rise
to tbe annual variation
Days
We also
tional
in France
to rule Out the eXistenCe
C.
storm
02 that contribute
electron
with the elevated
precipitation
oc-
by Dr. J. 1?. Noxon (private
communication),
neutral
but are somewhat
atmosphere
during
Some what similar
storm
33 hours.
Observations
S. C.,
and continued
level
of about 4.
commenced
lower
this night.
have been
seen
analog
support
around
tbe original
to a detailed
or from
later
(23-24
vertical
observed
and not caused
Winter-Night
The nighttime
of up to *2 hours;
temperature
companied
latitude
from
of the critical
foF2
temperature
was
particles
was much
we
which appear
produce
to penetrate the
27,28 who
by Jones,
ionization
increases
upon calculations
29
by Tanaka and Hirao,
It appeared
that the vertical
day,
of neutral
and Evans
hydrogen
as large
performed
however,
as
using
appear
a
to
diffusion
along
fluxes
3f
of ionization
suggested
into
that this
in tbe upper
atmosphere
avail-
however;
for example,
tbe
are possible,
day may have been influenced
by ambipolar
of the electron
the field
at Millstone
January,
considerably
lines,
by electric
as was assumed.
is anomalous.
of winter
in density
are always
local
and 20-2i
to the more
has been discussed
but there
accompanied
cooling);
in Nmax
November),
general
extensively
night pre -dawn increases
and peak near 0200 EST,
by increased
Increases
3-4 November,
which is linked
ionosphere,
features
at about midnight
to be caused
appear
to be:
are variations
hy a lowering
(3) tbe increases
ques in
“
of the plasma
are usually
ac -
of tbe layer.
is not confined
frequency
latitudes
30-31
nighttime
Tbe significant
the east coast
density
(e. g.,
This phenomenon,
of the winter
30” to 70” accordtig
are seen regularly
and Ottawa
was an
Elsewbere~i’14
increase.
fields,
was based
Other explanations
(2) the increases
dictions
in auroral
the time the measurements
has been contested
on the disturbed
on quiet nights
with a lowering
along
lower
on tbe disturbed
solely
commence
This phenomenon
curate
evening
cannot
calculations
1970).
near midnight.
(believed
values
the
to a
in the vane y region
and the electron
electric
fields
in tbe abundance
with O+.
be bavior
tion of the maintenance
4,43,32
earlier
papers.
The y usually
after
Behavior
regularly
commencing
March
re were
of a depletion
exchange
are observed
i i hours
carried
out on the post-storm
days, 25-26 March i969, have been subject
30,31
m which they were contrasted
with tbe behavior observed
during a
able to charge
D.
from
the density
March,
large
conclusion
detailed
some
that tbe flux of precipitating
explanation
by electric
This
More
the protonosphe
drifts
suggest
This
i.e.,
in the second
5 + for the following
explanation.
analysis
because
however,
of substorm
dusk.
September
exceeding
to have been present
on 23-24
findings
(-i 00 percent).
quiet day a year
(i)
These
of the layer
The observations
usually
appears
In this case,
than encountered
method.
the state of the
by which time the Kp index had subsided
there was an anomalously
ionosphere
that lifting
fields,
way at Millstone
that this is a manifestation
midlatitude
arose
at 2200 EST,
also.
On 30 September,
circuit
got under
less
lower
concerning
the night of 29-30
to Kp values
Soft precipitation
considerably
claimed
during
until 0900 EST cm 4 October,
order-of-magnitude
proposed
was observed
at 1050 EST and gave rise
until about 0400 EST.
during
by lack of knowledge
the event.
behavior
which commenced
hampered
to a small
geographical
to ITS predictions
for January
of foF2
of tbe United States
(45-N) to the north,
reported
which confirm
but appears
(Ref. 33).
Figure
1969 at 0600 UT (0100 EST).
can be seen.
(say north of 50° geographic
in the values
region,
from
Wallops
Island
pattern
5 shows
A ridge
region),
in
the P?e -
of increased
this map is probably
in this longitude
the general
39
While
to extend
increases
inac in
(37aN) to the south of Mi31s tone
of Fig. 5.
,...
EAST
..s,
PREDICTED
Fig.5.
The increase
temperature
content
stone
and consequent
geostationary
we proposed
by a lowering
in the layer.
than the peak density.
directly
that the density
The onset
tube to cool
of the plasma
AS a result,
the total
This can be seen in the Mill-
in measurements
following
conjugate
sunset.
Owing to the more
OCCW-S 30 mirmtes
later
Subsequent
and the onset
Studies
of heating
of photoelectrons
zemith distance
gate! heating
should
destroys
Figure
westerly
of total content
conducted
using
was tamed
6 shows
location
by a flux of cool
to be controlled
the time of local
of the conjugate
plasma
by the time
point,
from
it takes
and conjugate
local
the
sun-
midnight
there than at Millstone.
of the prod”cticm
,in the local
of photoelectrons
ionosphere
following
,into the magnetosphere
x ~ $OOO. If this is so,
this f tiding
increase
of this flux was supposed
set fOr MiJJstone.
ization
33
for January 1968.
satellites~4
Em_lier~2
escape
F2(MHz)
to be accompanied
of the electrons
percentage
and has been observed
the magnetosphere.
field
appears
redistribution
by a smaller
profiles,
,;;,
MUF(ZEROI
Ccmtcws of fOF2 at 0100 EST predicted
in Nmax invariably
increases
MEDIAN
be reduced
in the period
the earlier
should
then there
hypothesis.
arriving
Mmj”gate
mid-octobe
Meanwhile,
the conjugate ionosphere,
35
surmise
showed that the
be fully developed
is no time during
between
from
whenever
the solar
the night at which the conju-
r and mid-February
the question
of whether
(Fig. 6);
a flux of icm -
from
the magnetosphere
could produce an increase
in Nmax has been examined.
among
36
others,
by M ikhaylov
(who, however,
neglected
the change in the shape of the layer associated
with temperature
changes ). Mikhaylov found that a flux rising to -5 x 108 el/cm2/sec
appeared
necessary
to raise
aPPear to exist
The mom
foF2
from
at Millstone
general
flux of ionization
from
about 2.5 to 3.5 MHz.
in Sec. V, such large
fluxes
do not
at night.
question
of the maintenance
the magnetosphere,
of the nighttime
has been dis cussed
40
;—
As shown
ionosphere,
by a large
by means
zmmber
of a
37-42
of authors.
<5
I
X.90.
95
{00
405
1+0
,400~
DATE
fig .6.
Because
Contours of solar zenith
it has seemed
contributor
winds,
higher
levels
direct
experimental
maintaining
aPPears
where
E.
which blow toward
evidence
being
settled.
Disturbed-Nighttime
Millstone
be subject
lies
the equator
the existence
has recently
We address
it has been argued
at midlatitudes
and drive
(For
of significant
that the principal
of
along the field lines
43
) However,
to
see Rishbeth.
fluxes
at Arecibo,
further
months.
is the existence
ionization
review
been obtained
this topic
during winter
that would assist in
44
so the question
.
in Sec. V.
Behavior
in what must be termed
to changes
F-layer
rate is lower.
showing
F-layer
and its ccm@gate pint
is too small,
of the nighttime
the recombination
the nighttime
far from
x .at Mil Istme
that the flux available
to the maintenance
thermo spheric
angle
in association
sub-auroral
with events
latitudes,
taking place
and the local
in the auroral
ionosphere
may
zone to the north.
The penetration
of substm-m electric
fields into the midlatitude
ionosphere
at night has been dis 46
by Riister45;
and, by examining
ionosonde
records,
VanZandt, at ~,
Park~7 and
48
Park and Meng
have demonstrated
that these fields can penetrate a range of geomagnetic
lat-
cussed
itude of 20° to 60° during
an eastward
corrhng
hours
electric
about 9 hours
of local
time.
Prior
to midnight,
the layer
wbfle after titiigbt
it is usually lowered by westward
48
to Park and Meng,
these effects can be seen most clearly
during winter
of darbess
height with time.
field,
are lcxIger and the layer
These
vertical
motions
fl,mmally
“ndergm!s
of the FZ -layer
41
only small
changes
are usua13y accompanied
is lifted
fields.
nights
by
Ac-
when the
of shape
and
by changes
—
in peak density,
.% decrease
lowering
although
in the layer
of the layer
Observations
there appears
height
were
conducted
3),
8-9 December
ported
IV.
d.
Particularly
February,
AND
between
increase
Nma
in Nmax,
dis tm.bed winter
12-13
of these nights
their
February
appear
are the fluctuations
February,
some
maxFz.
but a further
on t 6.17
January
2.6-27 Febmary
of the effects
with substorms
(Kp =
i-e-
has not been
in hmax
which are associated
ION-TEMPERATURE
to exhibit
association
nights
(Kp = 3+),
and h
observed
on t 6-i 7 January,
with variations
in Nmax.
.RESULTS
General
Figures
electron
striking
and 26-27
ELECTRONA.
Several
magnetically
(Kp . 4),
hy Park and Meng,48 but at this juncture
determine
12-13
during
5-6 February
(Kp = 4-).
relationship
by an initial
to a rapid decay. 47
will give rise
(Iip = 4+ at 0000 hours),
to be no simple
often is accompanied
7(a) through
temperature
(z) and 8(a) through
(at 2000 K intervals),
vs height and time for the periods
temperature
-height
profiles
listed
(z) provide
and of constant
in Table
drawn hy hand through
diagrams
showing
ion temperatures
contours
of constant
(at f 00- K intervals)
II.
These diagrams
were prepared
the points plotted by the Calcomp
from
plotter. 5,6
(,1
Fig. 7(0-.).
Contours of electron
temperature
Te observed cm days listed in Toble Il.
42
——
.
r
.... ... .......... .. . .... . ...
.
. ...... .. ..
.,.
,.
‘.bw/z?n’-’A
(c]
Fig.7 (a-z).
44
Continued.
.
,..
P-----Q”””
-—––=2––
EST
(d 1
Fig. 7(0-z).
Continued.
45
/n
/ /
~... /
.l\!l\wL’’zz2=2’25f
:
~j
)d%’!?’
\-
T
-
ZS-Z7
1
‘EB
,
EST
[e]
Fig. 7(a-z).
Continued.
46
’969
/
—
I
/“
“0°
r
.
,7.23-24
.,.,,.,
am —
m, -
. ..~
:
:
m. .
400 —
m. -
*O. —
h)
.
Fig. 7(a-z).
48
—
-.
Continued.
,00
~aoo,,25-26
MAR ,96,
‘~[+
1
3400
4400
/////
Blti$v f’
‘o” 3200
3000
,00
4000
3800
3600
3400
3200
2800
;’””B\w@
,Coo
,600
\
i
2800
2600
2400
,200
40”h\w/@
2---G-G
~-.
,000
I
. ...
1
.?..
1
.400
I
..00
1
I
08..
100.
1
!2.0
,$,
1
!40.
(h)
Fig.
7(0-z).
Continued.
49
!
!...
1
!.0.
1
,0.0
I
,,..
2...
I
,
Km
Esr
[0
Fig. 7(a-z).
50
C.antinued.
I
01
fi9.7 (a-z).
Continued.
ll\3e00
)
“-36%-”/
II
1(--
.
1
1
EST
(k)
.,
~g. 7(a-z).
Continued,
52
—.
(1)
Fig.7(.a-z).
Continued.
53
(m)
Fig.7 (a-z).
54
Continued.
E,,
[.1
Fig.7(a-z).
Continued.
55
_-
303
t
(01
Fig. 7(IJ-z).
Continued.
....7
b)
Fig. 7(a-2).
Continued.
57
(Q]
Fig.7(cJ-z).
1
58
—.
Continued.
_j-$\q
, , g
203 —
600
....
m
....
---
. ..
-..
-~
-
1.~
1...
EST
1400
[r]
Fig. 7(.-z).
Continued,
w’!!
1600
1am
‘0”0
“w
2“0”
-Emz
, -.
..
[t]
Fig. 7(a-z).
Continued.
61
EST
M
Fig.7(a-z).
Continued.
62
u.
.
Fig.7 (a-z).
Continued,
I
,.
i
, ,,,
I
(w)
Fig.7 (a-z).
Ccmtinued.
I
I
{
,
(x]
Fig.7(a-z).
C.ntinued.
65
——
(Y)
66
(4
Fig.7(a-z).
Continued.
67
—
,Ca
Kc
b-?~
“
ma -
,Co
WC
me
,*CO
.-a
.Owa
o,~
EST
[.1
Fig.8(a-z).
Contours of ion temperature
68
Ti observed on cloys listed in Table
II
Tm@l.-
iv
,200
/
-00
220
2,00
2000
,(00
,,00
,,
30-3$,.,
1969
~
~
,800
, SOo
.Om
700
~
I
,,.0
1
!..0
EST
[b)
Fig,8
(a-z).
Continued.
69
I
$,,,
600
[
1
j...
zoo”
2’0”
-1
2“0”
.
B=$‘—r)\\/”
..0
“--4400
,Ca
:m~
J --—’=czx~
J
\
m
[c)
Fig.8 (a-z).
Continued.
?0
,. .;
,,
!500
, +00
4400
, zoo
n
//-s
1500
1300
,0.
~
4300
—
‘2-’5zN-si!5!ss-&’”
Tmm
,.0
m=@
2100
k,
,,00
80.
~
~e
2,00
,100
T800
,,,0
\ ,00
! ,.0
) SW
7..
,000
2000
1,0.
,800
,s00
,500
,40,
,700
,,00
A
,,00
—
/“
,,00
. .“
Fig. 8(cI-z).
Contl.ued
. . ..
.,
_ .-
.0.
L
~L
,..
‘“
,00
ESr
(*1
Fig, 8(.2-z).
Continued.
,0.
,KO
WC
L
,W
,,
24-22 MAR 4969
Em
!Wx
7..
(mm
600
=
!,00
Fig.8(a-z).
Continued.
73
.-
1,, z.,.
MAR ,%9
I
/2,00
fig, 8(a-z),
Continued.
74
T,25-26MAR
!,69
&&J,
moo
4..
,200
,00
,0.
800
!,00
700
‘0“-~
.m.
.2.0
0-.
...
.e~o
“m
‘Ooo
““o
EST
(N
Fig.8 (a-z).
Continued.
75
““c
..
=
E*T
[i]
Fig.8(a-z).
Ccmtin.ed.
Fig.8(0-z).
Continued.
77
Es?
[k)
Fig. 8(0-z).
COnf inued.
78
m,
(1)
Fig. 8(a-z).
Continued,
79
EST
[m)
Fig. 8(a-z).
Continued
I
‘1
80
,.
EST
(.)
Fig.8(crz).
Continued.
Fig, 8(a-z).
Continued,
i
,,
I
82
—
/
T, 9-10
4“.
1969
--IA
F*T
[71
Fig. 8(0-z).
Continued
83
I
///
,!00
7..
5.0 —
1
I
.. . —
3.. —
I
,..,
ES,
(q)
Fig. 8(.2-z).
84
I
Continued.
,,..
,40.
EST
[r)
Fig. 8(0-z).
Continued.
85
~
,
T, 2,-27AuG
,969
\\\
\\
>500
--’,.rn\
,~\W-q
8!
,400
*WC
/2500/
,
,..
I
“
2003
,X0
n
,8C9
! 700
‘7N===S3E!,,
/
/
m
EST
(s)
Fig, 8(0-z).
Continued.
86
J—
EST
(1)
Fig. 8(.rz).
Continued.
87
,..”
k
“k
w
,500
mc
,,<
t400
,7<
\
! ,00
700
\
,200
_-
m. -
\
800
700
6C0
,s,
(.)
Fig. 8(0-.).
Continued
88
.....-. .—-.. ..— .
..
.... ....:...-~a=.-a..-
r———————
EST
(V1
Fig. 8(a-z).
Continued.
.. .. ..i=.-..l.a.~-
.-
. .. .
.
., =,..,.,..
.,=, -
EST
(.)
Fig.8 (a-z).
Continued.
90
EST
(x)
Fig. 8(0-2).
Continued.
4,00
,400
f mo
\-
\vp’
EST
(Y)
Fig. 8(0-z).
Cent inued.
92
-G=z
EST
[z]
Fig. 8(0-z).
Continued.
93
Sin. e the lowest
downward,
point available
is for 225 km altitude,
and this was carried
The results
the exospheric
reported
out by assuming
shown in Figs.
neutral
it was necessary
a fixed
3, ?, and 8 have been
temperature
via thermal
va~ue Te = Ti = 335°K at t20 km altitude.
combined
balance
Quiet-Day
The most
dmsity)
arguments,
there
Electron
striking
feature
of the electron-temperature
is little
diurnal
variation
the Conjugate
in winter
of
have been
the night (Fig. 5), and this heat is lost by conduction
at the conjugate
On some
x small
nights
in Te.
after,
10-25
During
March
beginning
density
to the icrmsphere
through
botb
locally
than
February)
temperature
local
sunset
was usually
increased.
Thus,
gave rise
to only
seen to decrease
tbe temperature
change
at,
at
it is sometimes
possible
to discern temperature
insunrise, 9,35 provided that the local electron
density is suffi50
is not masked by the local cooling.
As mm be seen in Fig. 5, conlocal
and i 5 September
sunrise
another
0430 makes
of a temperature
increase
beginning
hut in this case
it difficult
margin
to be certain.
beginning
only during
The temperature
of conjugate
somewhat
before
the temperature
Similarly,
before
(’l to 2 hours)
approximately.
[ Fig. 7(f)] is an example
increase
instance,
by a useful
– 4 October,
at about 0300 on 22 ‘March
[Fig. 7(h)] represents
nea?
This
to the prdtcmosphere
equinox
that the electron-temperature
beginning
so that heat is supplied
with conjugate
(Xconj > i05~) precedes
sunrise
to the
in summer.
the length of the day is greater
i2-13
electron
as the electron
low so that the effect
POSsihle
5-b February,
The winter-night
marked.
associated
the period
on the other hand,
(e. g.,
midnight
dawn was more
creases
In summer,
smdit
variation
point (Fig. 5).
winter
decrease
‘- or shortly
point remains
is that (in contrast
diurnal
throughout
ends of the field tube.
dication
and tbe results
behavior
and a large
in winter
crease
variation
Temperatures
is because
jugate
to obtain the diurnal
in Refs. 22 and 49.
B.
ciently
to extend the curves
heating.
at local
that there
dawn cm 24 September
It is
0400 on 26 March
increase
it appears
in-
[Fig, 7 (“)],
sunrise
is some
in-
but the ef -
feet is not pronomrced.
A consistent
close
feature
to or somewhat
ples are provided
ceeded
-i.5
of the daytime
hmax F2 whenever
above
by 26-27
February
x 106 el/crn3.
temperature
electron
and 25-26
As we move
temperate
the local
March
away from
is the minimum
cooling
becomes
which were
sunspot
large
occasions
maximum,
produced
enough.
at a level
Exam-
when N~axF2
instances
ex-
of electron-
become infrequent at Millstone,
as the required
high electron
densities
5,6
am no lrmg’e r encountered.
For the same reason,
the probability
of encountering
a tempera5%
ture inversion
has always been considered
to be higher in winter than in summer.
During i969,
howe”cr,
inversions
there
were
during
sumet.
worthy
that cm these
less
These
include
During
because
winter
the local
6 May,
a“d the local
cooling
i-e
density
beating
the electron
serves
This
30 May,
5 June,
from
is particularly
encountered
1 July,
varies
of the inversion
rise
particularly
It is note-
was typically
(-25
correspondingly.
with the electron
caused
for example,
a little
to 30 km) higher
would be lowered
inversely
the ternperatuv+
pronounced,
in smmme?,
and 23 September.
was substantially
photoprod”ction
temperature
to modulate
were
at the level
the peak of the layer
IIowe”er,
nights,
Cmrn tk,e protonc,sphe
days m which inversions
days the electron
than 106 el/cm3.
than found in wi”tei-,
4-5
several
by heat
on i 6-17
density
conducted
January
and
November.
94
., . .—...——..- ...———----
C.
Disturbed-Day
Electron
On the disturbed
increasing,
suggesting
began
that it was caused
hy the growth
of the F2 -laye?
. i05°)
night,
Te increased
in the valley
occ”ming
During
density
a mininmm
(near
remained
+00 km).
above
was initially
its normal
in the valley
flux.
after
midnight
However,
the night,
value at most
region
to be
levels.
(near 250 km),
Thereafter,
the temperature
to have been caused
appears
it is possible
to the lowering
observed
tht
that conjugate
sunset
of the temperature.
250 km as the F2 density
high throughout
geomagnetically
disturbed
near 0120 EST that appears
suggesting
declined.
After
Tem~
mid-
ratures
that the soft particle
The temperabm-e
in the valley
at Oi45 EST.
urements
are too low owing to the neglect
than on 23-24
the results
March,
However,
(Sec. 11-C).
flux was
as high as 300 km is provided
at the commencement
have arisen
from
assuning
evidence
hy the large
of the observations
region
beneath
it is possible
ions
variation
m 23 March.
that only 0+ ions were
density.
of conjugate
the layer
that both sets
There -
sunrise
peak was sub-
of temperature
(02+, NO+) at these
that molecular
- i October),
the next 2 hcmrs reaching
as a consequence
of molecular
Some
(29 September
during
with a. peak in the F2 -region
possibly
less
period
and declined
to coincide
stantially
interpreting
observing
began,
gradua13y increased,
occurring
ions were
levels
mess -
when
abundant at altitudes
of ion temperature
below
this level
This is thought to be unrealistic
and to
pi-eserd.
Ion Temperature
The ion temperature
below
shortly
high when the observations
the temperature
D.
encountered
at 2200 EST contributed
the second
.a minimum
perhaps
temperature
at all times.
Te was already
after,
electron
again at all levels
region
the electron
by a peak in the precipitating
and reached
(Xconj
March,
a peak near 2130 EST when it was twice
with the highest
to decrease
present
night of 23-24
and reached
This coincided
Temperatures
300 km where
the ion temperature
and the neutral
[Figs.
8(a) through
(z) ] exhibits
the ions and the neutrals
increases
exospheric
only a small
are in good thermal
and takes up a value intermediate
temperature.
As such,
diurnal
contact.
between
it tends to mirror
change
At higher
the electron
the changes
at altitudes
altitudes,
temperature
in the elec -
tron temperature.
v.
VERTICAL
A.
IONIZATION
FLUX
RESULTS
General
The new spectrum
analyzer
installed
vertical
velocity of the plasma over
pre~ented.30>31,52,53
As discussed
to the direction
of the magnetic
field
line.
the sum of a component
v ] 1 parallel
oriented
in the magnetic
‘ohs
= 0“96 ’11 + 0“28 ‘1
In the F-region
the drift
velocity
VL NS = EEW/B
v
permitted
the first
Preliminary
results
in Ref. 30, the antenna beam
magnetic
field
in i968
20
Millstone.
The observed
to the field
1 NS
velocity
and a component
NS direction
reliable
from
is directed
estimates
of the
this work have been
at an angle
vob~ may be considered
v ~ NS pe?pendimla.r
of i6to be
to the
where
(41)
NS
will be controlled
by the east-west
electric
field,
i.e.,
{i2)
.
95
—-
Separate
measurements
which indicate
by ignoring
that,
made using the L-band
except
during
the V1 component,
magnetically
it is possible
with errors
‘e=surements
independent,
‘f ‘1 I
it is sometimes
The most
useful
radar
directed
to regard
possible
to remove
these
19,54
have been made
the observed
Thus,
v 1 NS < 30 111/s~C.
velocities
as providing
Sinc,e the v
component
disturbed
of up to *<O m/see.
obliquely
conditions,
.L
will be height-
errors.
the measurements
of the vertical velocity are estimates
of
30
the N-S component of tbe thermospheric
wind
and of the ionization
fluxes exchanged with the
53,55
magnetosphere.
Since the determination
of the winds is cw-rently
tbe subject of a separate
56
study>
we confine our attention here to the question of the magnetospheric
fhx.
A limitation
height
re suits from
of the drift velocity
of the transition
to measure
directly
altitude
forhmately,
.-
H+ fluxes
height
of the layer
altitudes.
by pressm.e
(e. g.,
Similarly,
10SS) or expansion
vertical
protonosphere,
ratio
reproduce
the observed
ratio
at altitudes
are reflected
in tbe vertical
(under
in plasma
drift
in the
at all
and
also establish
of ionization
of the fhx
hmax F2
changes
of production
temperature)
on the excba.nge
disti-ib”tion
Thus,
the influence
Lln-
well above
below.
of changes
the velocity
of a geophysical
as well as to reduce
and hence
ion. 30
the predominant
in the plasma
winds)
to the great
when Ne,
with the
Te,
and Ti
of time.
to average
fluctuations
owing
it is not possible
only the flmxes of the 0+ ions
of tbe ionization
of the layer
to study the altitude
results
natm-e,
the uncertainty
it may be noted that the standard
P5/Pn,
P~/Pn
of neutral
(as a re,wlt
for a period
(TIDs),
drift
yield
0+ is always
to obtain information
it is desirable
to remove
nection,
since
occm-ring
and decay
in order
it is easiest
aPPear to be constant
Disturbances
as a result
the growth
Thus,
In practice,
changes
and contraction
fluxes.
in part,
are present),
is that,
km) at this latitude,
the ohservatims
as shown in FWf. 34, the vertical
tends to be controlled
made at Millstone
0+ and H+ (-2000
Instead,
the H+ thx.
(even when significant
measurements
between
deviation
e.g.,
obtained
caused
OVer a number
by Traveling
in the (noisy)
of runs,
Ionospheric
estimates.
in this con-
in the results wmies with signal-to -noise
52
An empirical
result which appears to
on both height and time of day.
variatim
for the results
of the rms
presented
deviation
with the pr-edet ector
signal-to
-noise
in Ref. 52 is
A“=%103+
+r’z‘/’”
where Vi is the mean thermal
observations
(pdses
).
range
5 to 20 m/see,
fore,
it is essential
interval
the 8-minute
to average
over
the contours
to be roughly
ity were
computed
the velocities
Ods listed
constant
using
observed
in Table
VI.
to the tme
runs,
which the densities
-Height
three,
drift
i/2
v.
and temperatures
VI).
or five cycles
these
To obtain
and this r-eq”ires
reliable
appear
of independent
lies
results,
the existence
in the
there-
of a time
constant.
i“ Figs. 3 (a) through
near noon and midnight
by day and by night.
fn plotting
Av typically
Profiles
with time (Table
four,
, and n is the number
at Millstone,
of dens!t y and temperature
we have been able to find periods
aPPear
runs conducted
mm r several
Steady .State-Velocity-vs
By examining
of the ions (2kTi/mi)
and is comparable
of i or 2 hours
B.
(Z),
For
speed
(13)
Similar
diagrams,
96
For
when the density
these periods,
of data.
diagrams
Figure
profiles
9(a-b)
of w+rti.al
presents
were comtmc ted
the height assigned
(z) and 7 (a) through
and temperature
to each
w+loc -
examples
of
for all t!,c peri data point was a
TABLE VI
PERIODS
Date
(1969)
16-17 J.snu.a,y
EMPLOYED
FOR COMPUTING
AVERAGE
VELOCITY
PROFILES
Daytime
Nighttime
(EST)
(EST)
1200-14&3
VERTICAL
Comments
2200-2330
AWB= +7 m/4ec
0130-0230
As above
10-31
January
5-6
February
1300-1500
2330-0100
As above
12-13
February
1500-1630
2300-0100
As above
26-27
Febr..ary
I 330-1530
0000-0200
As above
21-22
March
2300 -OICO
,% above
25-26
March
9-10
AK.ri I
1200-1400
2300-0100
As above
23-24
April
0800-1000
2230-0030
AWB = O
6-7
May
2230-0030
As above
1200-1400
As above
30-3 I May
0930-1030
As above
June
1000-1200
As above
June
1 I 00-1300
0100-G200
AWB = –7 mjsec
July
I 130-1300
2330-0030
As above
I -2
June
5-4
23-24
I -2
9-10
July
29-30
July
14-15
August
—
1000 -I2OO
0000-0130
1000 -1200\1200-1400
As above
As obove
As above
9-10
September
I 330- I 500
23-24
September
0900-11
14-15
October
1300-1500
As above
3-4
November
1400-1530
As above
20-21
November
1330-1530
1030-0230
As above
8-9
December
1300- I 500
?300-0130
As above
As above
oil
9030-0300
97
As above
,C+4
/
‘ooor71zEELI
,6-17 JAN!969
2?CU -23,0 Es.
-.ln
.00
❑
we
o
z
.
:
0
‘+
I
o
u MODE OW,. -7WSOC
❑
c .00,
A.c=-,om,’,c
.m
,
.~
“,,7,,,, “!,0,,,”
_-
1
.
B .0.9,
4.,.
+7.,,,.
m c . . . . ..,.
-)0”,,,.,
1
1
-4.
“,RTI
I
-a
(./..,)
-m
CAL
,,,.eighted
Exmnples of plots of aver.ge
height,,
matched-filter
that takes
response
echo power
vs delay.
distribution
ob~erved
The error
bars
and serve
to indicate
nighttime
curves
these
plots
signals
during
the scatter
is that introduced
where
reading.
tbe receiver,
smaller
source
arising
of this error
the echo -power-vs
of
-delay
of the points
of error
is discussed
between
and
in constructing
the input and output
of the fall in the applied
in the Appendix
means,
for the daytime
encountered
difference
as a result
about their
where
voltage
it is shown to
For typical
These
(14)
‘/s’”
DC current
read on the transmitter
values,
Vm = i 00 kV,
this by me.ms
and the receiver
In plotting
tests
of tests
tuning was adjusted
gave an estimate
meter,
and Vm is the transmitter
Iav . 3.8 A, Aw -–i
in which the transmitter
to balance
of AW -–10
tbe “elocities
in the C-mode
the results
in the height
the varying
ccmdition
[Fig. 9(a-b)],
and a correction
interval
where
of the B-mode
a correction
2 rn/sec.
signal
the power
m/see
Attempts
was leaked
observed
in the C-mode
of –iO m/see
for the B-mode
the results
filter
into
at the center
and a somewhat
was applied
to all tbe points
data was sou~ht by attempting
overlap.
bank during
98
__
distribution
value fm. the B-mode.
gathered
3
,,
using
deviations
in the phase
amplifier
by the Pulse and
measurement.
these may be taken as typical
A second
by the change
klystron
io81av
—
~Vm)3/2
have been made to verify
pair of filters.
are the rms
imposed
and (2) the actual
computed
(A-mode)
for periods listed in Table VI,
weighting
function),
were
iOO-Psec
of the data;
The magnitude
Iav is the average
voltmeter
( 1) the triangular
heights
for 1969.
constructed
of
Av/=—
I
weighted
velocities
ambiguity
shown in Fig. 9 (a-b)
constructed
the pulse.
the radar
in the preceding
at the transmitter
be of the order
.ertic
tito account:
(i. e.,
These
,./,$.1
(b) MGHTT,ME
10) ,,”7,.,
Fig. 9(a-b).
“Em,,, ”
This
the year.
procedure
seemed
to match
justified
by
.
t
Tmi@L
.
“t
t
I
I
I
J..
I
,,,
. . .
I
I
I
,,,
.,”
I
,“.
,.,
,,,
I
I
I
I
...
,0”
m,
,,,
I 969
Fig. 10. Estimates of bias errcms in B-mode results breed on matching velocities
t. those .bserved
in C-mode in region of oved.p.
Estimates have been confined to nighttime,
m velocity
is then
les$ rapidly varying with height.
AISO shown (solid line) is correction Iraw finally adopted,
Figure
finally
10 shows
adopted.
it difficult
to detect
be considerably
C.
Velocity
true seasonal
from
there and diffuse
created
there
upward
diffuse
variations
well above
downward
is usually
line is the correction
tbrou ghout the year
at low altitudes
the day the drift
tbe level
to lower
and are lost via charge
upward
At night [ Fig. 9 (b)],
into the magnetosphere.
the drift
the magnetosphere
below
(unless
which renders
these happen to
about 500 km is downward.
of peak production
altitudes
a transition
where
to upward
exchange
53>55
(near
chemical
drift.
Ions created
with hydi-ogen
at all altitudes.
with atomic
creates
a flux of 0+ ions which diffuse
at a rate that just balances
down through
their
the layer
rate of arrival
peak to levels
(at times
Between
this transition
The protons
There
oxygen
readily
holds.
above
atoms.
tends to be downward
from
{80 km) cannot
equilibrium
which charge -exchange
protons
removed
The solid
variation
in the drifts
Fig. 9(a) that during
ions created
500 and 600 km,
diffuse
in this manner.
Results
It can be seen
level
of AWB obtained
this has a systematic
larger).
This is because
be lost
the values
Unfortunately,
so
is then a. fhx
above
where
when the layer
of
hmaxF2.
This
the ions are
is stationary
and stable ).
D.
Daytime
The plots
vertical
Flux Results
of vertical
flux for daytime
velocity
[e. g.,
and nighttime
the velocity
was assumed
importance
on the interpretation
to follow
Fig, 9(a-b)]
periods
have been employed
listed
the smooth
curve
of the velocity
in Table
VI.
[ Fig. 9 (a-b]].
results
to construct
In conr,tr”cting
This
at the highest
places
altitudes,
graphs
these
of
plots,
considerable
especially
during
the daytime.
Plots
of the daytime
The downward
flux appears
fluxes
obtained
in this
to i-each a maximum
99
manner
close
are shown in Figs.
to the F-1ayer
11 (a) through
(t).
peak that lies in the range
‘m lmm
16-17
t
JAN
,200-,400
1969
EST
~
I
.,
,00,0
I
‘:F
L
L+-_+-
.,
(.1/..2/,..)
(al
FLUX
.
)
,1
1
,8
‘oG).
‘Lu;b~l/cm’/lac)
Fig, 11(0-f).
Daytime vertical fluxes computed for periods listed in Table VI.
AISO shown in some
cases cme ‘correcte
d,,cuwes which have been obtained in rn.anner outlined in te. t (plus signs indicate
upward flux;
and minus signs indicate
downward
%00
.
flux).
,,00
,00
1.
26-27
r-
‘“” -
-lima
25-26
FEB 1969
1330-1530
MAR 1969
1200-,400
EST
so,
EST
t
I
.,
,s3
LWO
‘Lu;d~@/secl
LOG,,
FLUX
(,1/..2
(e)
,000
TIm!EL
,00
I
9-,0
,,,
,,6,
1200-1400
EST
,
LO.,.
,,”.
(,1/.. %,)
(f)
Fig, 1I (o-t).
i 01
Ccmtinued.
J,,
-.1
,
.
MU, suwo
o
CORRECTED
I
I
.,
,,
c)
,0.
1
5-6
JUN 1969
1000-1200
EST
.,
LO G,,
FLUX
{.$/< .2,s,.)
LOG,.
[n]
{WC.2A.C1
FLUX
(i)
Fig. 11 (o-t).
Continued.
23.24
WN
1100-1300
,969
EST
800
~
1
1-2
-m
1
-,
(,,/..,,,
FL”,
EST
t
1
+,
LOG,,
WL ,969
1130-1300
-s
r
am—
(k]
-imIEL
3-10 AIL 4969
1000-1200
E?,,
600
z
~
:
g
!
..0
200
~‘<
o
1
-m
[M,
m%,d
LOG, O FLU,
Ii)
,0,0
.,
-,
,,
-8
‘Lu:l
p/cm’/,ecJ
‘o%
F;g. I I (a-t).
f 03
Continued,
,.
.
.. ..
.-
r
‘“ -E!zml
1000-1200
\
c
14-15 AUG 1969
EST
\
>
Bce-
:,=:
:
g:
.Cc F
.
MEASURED
o CORRECTED
=0?
,,
I
-9
I
..
,,
-,
1
,,
,
-,
LOG
N FLU:mV2/OOC )
,
I
,,
-8
‘Lu:n~/cm’/5ec)
L%
,mu
TEEliL
o
9-10
SE,
,969
1330-1500
800 –
EST
o
,.
?
: m.
—
o
:
q
%
WC —
*W –
I
-,
I
I
-,
I
-7
,0610
,,”,
,6
(e(,m,,,ed
(0)
Fig. 11 (a-t).
104
I
l—
Continued,
,7
,
..
.
ME AS” FED
o
CORRECTED
t
,~~
1
.
.,
Lo,%
‘Lux {cl/cm
‘,. (Q)
!., )
—
Tmm_
o
,00
I
14-15
OCT 1969
1300-1500
3-4
EST
Nov 1969
1400-1530
EST
[
—
Fig. 11(.-t).
Continued,
105
I
,W.3
,,0
j
TmEm
20-21
NOV 1969
,330 -,?,30
ES,
-
,W _
-#
2
:
Y
4C0
,Ca
~
c
1
.,
,ma
=
m,
I
8-9
DEC 4969
1300-1500
EST
~
LO G,, ,,”,
,., /.”,%
[1)
Fig. 11 (a-t).
—
Continued
The upward
1 to 6 x 109 ellcrnzlsec.
flux is usually
value in the range 2 x 107 to 2 x iO 8 el/cm2/sec.
decrease,
atom~.53
pears
and this has heen attributed
However,
in some
to be increasing.
fn two cases
under
[Figs.
plots
examination.
These
resentative
appear
to be cases
curves
considerable
have plotted
from
of daytime
variation.
(in Fig. i 2 ) the altitude
(against
flux
a scale
to vary from
day to day in a correlated
with respect
in others
it ap-
throughout
the altitude
range
was computed
for a
are not considered
rep-
profile
two cases
analysis.
flux [Figs.
Ii(a),
to see if this exhibits
of the transition
peak upward
of the flux curves
vertical
with hydrogen
while
may not be well determined.
in which the velocity
further
In order
variation
These
e.xcbange
of altitude,
to be downward
flux was absent.
and have heen excluded
The remaining
display
that the altitude
600 and 750 km at a
the 0+ flux often is seen to
charge
independent
the flux appears
time late in the day when the escape
this level,
to the 10SS of 0+ through
the flux appears
This suggests
1i (c) and (r)],
found to peak between
Above
that imreases
between
toward
fashion,
to the abscissa.
(b),
(d) through
any particular
upward
bottom).
(q).
and downward
These
(s):
and (t)]
regularity,
we
fluxes
two quantities
suggesting
that there are errors
This could
be the result
and the
appear
in the location
of an additional
bias
,00
-
0
PEAK
x
,,.,
UPWARD
FLUX
ALTITUDE
s,,,0,
– 800
error
Fig. 12.
Values of log peak upward flux observed in pl.ts
between
upward and downward
in the velocity
outlined
above,
through
vertical
through
details
at all altitudes.
as an instrumental
motions
averaging
over
Ev=lls
several
foregoing,
effect
cycles
(e.g.,
(e. g.,
of data.
in flux above
it seems
with the observed
Indeed,
in order
postulate
an H+ abundance
to acmmnt
of the order
arise
altitude
casts
as
chirp),
or
doubt on the accuracy
to compute
decrease
i970.
fn view Of tbe
by the accuracy
in the 0+ flux,
0+ at 900 km (Ref. 55).
of the
one is obliged
such a large
407
i
of
the H+ distribution
in 0+ flux for 24 March
may not be warranted
of iO-percent
for frequency
fields
altitude.
have attempted
for a significant
of electric
that have not been suppressed
This conclusion
decrease
as a result
compensation
by TIDs)
the transition
that this type of calculation
results.
could
improper
caused
and Holt53 and Schunk and Walker55
that would be consistent
,.
Such an em-or
of the layer
such as the decrease
of Fig. 11, and transition
FIu. regions.
—.—.
,,.—.,...—.,;..—
to
abundance
percentage
in cmr reWlt.;7
i 000 km,
and hence
in the region
layer
peak should
Accordingly,
mine
all escaping
increase
Figs.
charges
will be carried
That is,” we propose
to a constant
by bias errors
value,
but appears
transition
altitude
by atomic
that the upward
flux and V* is the bias
velocity
error
well abcwe
oxygen
and the altitude
in the vertical
to be absent
lies
(i.e.,
as 0+)
flux above
variations
the
seen in
that have not been remcved.
in the velocity
curve,
then the
Ne is the electron
against
4 4(g),
density.
(m),
BY plotting
and v! (the slope).
to vary markeddy
the electron
dc. exhibit
(i5)
- F, + iVevV
obs as a function
Curves
Figure
of i4-i5
i 3 shows
August
of “corrected”
the corrections
flux values
of Ne.
T“tis has been attempted
for the. case
large.
(n); and (p) irhere
upward
Fobs
with altitude.
density
to have been extremely
curves
on the spectrum,
the O+/H+
flux is
F! (the intercept)
plotted
positive
if Fe is the true escape
ward flux appsars
pears
its effect
at Millstone,
with height
i.atroduced
F
where
that,
which we are able to study.
Fig. i 1 are chiefly
observed
could be seen through
We conclude
in those
values
constant
cases
tO deter-
where
of the ohserved
1969 when the drift. error
flux “[Ne(vob~
are largest.
that are sensibly
it is pOssible
the upflux
Vt ap-
– V’ ) ] are shOwn in
It can be seen that the ncorrected”
over
the altitude
range of interest.
,..’.
./
~~
N, WC.3
Fig. 13.
Figure
Ne in region of upvard
flux for
1000-1200
EST 0. 14-15 August.
Slope of line gives magnitude of velocity
required to cause flux to be height-independent
over this interval.
bias v’
i4(a)
tion in those
cases
been reduced
from
presents
be height-independent
change
Plot of &served
in the region
where
a factor
flux
our best
F vs electron
x 105)
estimates
it was deemed
ues of Fig. 14(a) are lower
of the upward
appropriate.
correct,
to the flux.
Ignoring
i 08
of 4.
making
The assumption
in that some
1000 km must take place,
limits
flux after
the above
It can be seen that the spread
of 10 (Fig. 12) to a factor
may not be strictly
below
density
Thus,
loss
the cases
in values
has
that the flux should
of 0+ through
it appears
correc-
charge
that the ‘corrected”
in which a corrected
exval-
flux curve
,.
has been
-
obtained,
we get an average
b, taken as our. best estimate
tion heights
for these cases
proximately
to an exospheric
value for the escape
of the daytime
was 600 km.
escape
Adopting
temperature
flux of 5 X 107 el/cm2/see,
flux during
a scale
of 1000 K),
i 969.
height
we require
The average
which maY
of the transi-
H = 60 km (corresponding
the production
ap-
q at 600 km
to be
q600
The values
quite large,
F!
~
.
. 8 el/cm3/sec
of the peak downward
but,
flux obtained
if the 71corrected’!
points
I .
are shown
are ignored
0,$ ERV5D
JAN
FEB
[.-”
MAR
A,n
amounts
Here
the scatter
to a factor
mu.
I
1
‘A”
‘UN
I
I
I
‘“L
‘“G
““
1
I
.0.
me
“
,,6,
(b)
Fig. 14(a-b).
Values of log peak flux obtained
points) or after correction (open points).
f 09
from cuwes of Fig. 1 I directly
remains
of 4, and an
~ 7.721
I
I
I
I
-8,,
vALUE
in Fig. i4(b).
again,
c,AY,,
ME“,.,.,
~
,,0
(i6)
.
(closed
TABLE WI
CURVES AVERAGED
AND SUMMER
TO OBTAIN
MEAN WINTER
DAYTIME
FLUX CURVES
Summer
Winter
16,-17 January
23-24
April
5-6
February
30-31
May
14-15
October
5-6
June
20-21
November
1-2
July
8-9
December
9-10
July
’00”TmEL
r--”
WERAGE
DAYTIME
VERTICAL
FLuXES
1969
)
, / /’
/
(’
I
‘\
(
/
/
/
/
/
/
/“
,“M.,,
WINTER-,
~
--J-+._
‘O%.
‘Lux
2“k{cm‘“c)
,!
Fig. 15.
Averoge
flux curves obtained
by taking
for five days (Table Vll).
10
mean of (uncorrected)
curves obtained
ave rage value for the peak downward
is somewhat
variable,
the flux should
but usually
decrease
lies in the range
linearly
over
divergence
the 300 -km level,
we can make an estimate
negligible
(since
should
roughly
the peak production
we estimate
lies
that the average
3 X 109 el/cm2/sec.
Employing
While
this appears
consistent
close
must commence
do not consider
curves
five
and five
and the differences
flux in winter
ing as a result
the curves
the flux would be -3
E.
Nighttime
Vertical
listed
in Table
Vf.
Except
i6(a)
rates
processes
and resembled
error
pertaining
fields).
loss
(n)],
The losses
the upward
level,
i.e.,
where
it reverses
bias errors
(Fig. i i).
Vlf,
flUX
at about 550 km.
sign,
in the velocity-vs
we
different
from
out for
that are presented
the estimate
to be significant.
arrived
in
at above,
The peak downward
This is probably
By extrapolating
summer.
-altitude
This has been carried
with results
in summer.
during
July,
of Fig. ‘11 were
all cases,
of the layer.
fluxes
a real
the linear
effect
aris -
portions
of
of losses
It is clear
gravity
(which,
by 0+ ions
of altitude
well below
over
the interval
periods
and uncertain,
these
created
the O+/H+
Fig. 9(b) that there
the drift velocity
to decay
can be
at a rate set by the
by the competing
by neutral
winds and possibly
by H+ diffusing
downward
transition
to be small
from
the protono -
and should
region.
nights
give rise
The altitude
in only three
600 to 800 km for these three
at
is small.
is governed
caused
will diffuse
400 to 500 km was observed
poor
F-1ayer
in turn,
and lifting
The 0+ ions so created
from
where
the nighttime
of the layer
will be offset
appear
for tbe nighttime
the flux was found to be downward
at low altitudes
we expect
under
constructed
when the results
In almost
of the flux shown
(as a conseqwmce
the loss
those when the decay
.
Rather,
58 it is ~ot
cases
[ Figs. t 6(b ),
we obtain
an esti-
flux of 2 x 407 el/cm2/sec.
variation
was descending
ward motion
the region
of the large
in Table
to those
the shape
diffusion
and averaging
able to balance
we obtain
at this level,
flux.
the 300-km
are not considered
(n).
at the altitude
of the flux above
The altitude
this ap -
in both seasons.
for 29-30
conditions,
mate for this arriving
layer
above
to be little
rates
similar
to a flux that is independent
(m),
to
would be
400 and 500 km down to 300 km we find that in the absence
into the ionosphere.
variation
region
were
Adopting
of losses
flux,
production
through
that observed
in the nighttime
of downward
electric
sphere
some
listed
the curves
through
Under steady-state
loss
if loss
Flux Results
shown in Figs.
considerable
heights
of the flux curves
X i09 el/cm2/sec
flux diagrams
all altitudes
scale
appear
to be twice
of the greater
for the escape
of F-region
the flux curve
days
fluxes
in Fig. i5 between
this altitude).
300 km in the absence
of 600 km for the upward
several
between
appears
this linear
there,
produc -
to be serious.
‘rsummeru’
The peak upward
below
from
exist
the log of
where
(17)
to removing
(Fig. 9) is to average
‘twintert!
Fig. f 5.
are
. 4.i5
in drawing
approach
substantially
estimates
this inconsistency
An alternative
Extrapolating
balance.
the peak,
.
altitude
in In (508/8)
fn view of the difficulty
Above
of the peak flux
of about 350 to 500 km,
of the flux that would
Eq. (i 6 ) and allowing
to current
with the transition
250 to 300 km.
region
flux through
q300 = 508 cl/cm
!
the altitude
tion and downward
preach,
The altitude
flux is 2.5 X 409 el/cm2/sec.
in the remaining
of loss),
at this time! (despite
rate appeared
due to an eastward
small).
electric
i.e.,
plots
the flwi from
of Fig. !6 suggests
that the
the magnetosphere
was not
the fact that the periods
An alternative
field.
fn either
explanation
case,
a large
selected
for analysis
were
is that there was a downpart of the fhx
observed
m
1“0 -
16-17
JAN
2200-2330
800
1969
EST
30-31
JAN
0!30-
0230
1969
EST
400
\
200 [
I
ASYMPTOTIC
FLUX
(600
= -1S
,.900
X 10’e!lcm21s0c
km)
,
‘OGIO
‘Lux(o~1cm2fs’c)
,
,.
(b)
1000
,m
-!18{4
-11
118.2
5-6
FEB
118-2-119711
12-13
1969
2330-0100
FEB 1969
2300-0100
EST
EST
800
:
600
k
:
*
400
,.20
“L
1
:)
ASYMPTOTIC
FLUX
(500
AsYMPTOTIC
i
FLUX
= -4x107
el/cm2&
= -5
X 107dh2/sec
t0700km1
t
,
150010700km1
LOG,.
FLUX
(dcf112/9.C)
(d)
Fig. 16(.-.).
Loglo vertical
flux .s altitude
observed for nighttime
t i2
periods listed in Table V1.
1Oca
[18-2
21-22
-11913[
MAR1969
2300-0100
EST
8CQ -
~
600 -
!
g
:
.Ka
-
ASYMPTOTIC
200
FLUX
(500
= -9
x 107el/cm2/,
to700km1
t
I
-,.0
,
-7.0
1
- m
LOG,O
FLUX
-
I
-..0
LOGIO FLUX
(CIICMZISEC)
[.1 Icm’lsnc)
(f)
[e]
1000
-tiEEI@
23-24
APR 1969
2230-0030
EsT
0
*OO
;
.00
i
~
:
400
‘
?00
ASYMPTOTIC
FLUX
(600
= -4.’4x
107el\tm’/w<
/
,00
ASYMPTOTIC
to OOOkml
FLUX = -2
(4501 .700
x 107 el/Cm
km)
t
[
I
I
-,0
,
-,.0
I
-,.0
LOGIO FLUX
(e!/cmz/=C)
(h)
!
Fig. 16(.-.).
.
Continued,
Z/%eC
e<
1000
118-2-119161
23,24
JUN
1969
0100-0200
EST
*OO -
:
ma
0
–
:
:
:
4C0 —
I
z00
‘“”~
-,.0
FLUX
(500
= 9 X 10”e!/cm
2/w
to 800km1
t
-8.0
LOG,O
ASYMPTOTIC
-7.0
~
-6
{,l/cmz/see)
FLUX
LOG, O FLUX
(,1/..21$,,1
(i)
(1]
,030
118-2 -1191s1
6-7
MAY 1969
2230-0030
I
800
o
/0
1-2
,---
JJL 1,69
,330-0030
E*T
/
.
-
,00
–
‘
z
5
z
<
EST
600
;
i
z
:
I
J
x
W.3 –
400
(
,00
200L—____—
t
~~
-,.0
.8.0
-7.,
Lo,,.
,,”.
-,.0
-..0
-7.0
-8.0
LOG,O FLUX
{,,/,../,.,,
[.1
(i)
(k)
Fig. 16(a-n).
ii4
C.ntin.ed.
/..2/s..)
-6.0
,000
‘“””v
I 18-2-119181
8-9
DEC 1969
23CQ - 0130
t
L
200
t
,
~
-9,0
-6,(
LOGIO
FLuX
(.,
EST
/,m2/,,c)
LOG,.
(n]
(ml
Fig. 16(a-n).
will be caused
by the descent
be given an eqw.tion
of the layer
of the form
If this is the case,
sphere.
be carried
below
out for the altitude
to sensible
to compute
values
region
it was applied
layer
was clearly
descending
cases,
plots
in only 8ix cases
stationary,
of the values
estimate
and appears
for the, arriving
the results
sensible
are sufficiently
which
thereby
Since
reliable
vs IXe.
Fobs
casting
in Table
losses
the method
sensible
appeared
some
to permit
However.
reaulta
firm
conclusions
listed
(i.e.,
in Table
VI lead
for nights when the
for five of these.
linearly
doubt on the validity
fluxes
this must
are important.
constructed
to depend
are plotted
will
the protcnm-
does not depend upon the layer
VfII is 3 X i 07 el/cmZ/sec.
the two methods
flux Fobs
from
flux is fully established
fm. which
flux diagrams
in the light of the escape
from
Fobs
vs Ne for the other nights
VfII).
VIII) and yielded
over
of F! listed
flux obtained
the region
of Fobs
(Table
( Table
this was quite restricted,
average
by plotting
for a fm-thei- seven
range
v,) so that the observed
F, is the true flux arriving
in which the protonospheric
and above
FI from
VIII is the height
(with velocity
of Eq. ( i 5 ) where
region)
being
in Table
Ccmfinued,
F9 can be recovered
the change-exchange
Attempts
(d /Cm2/SOC)
FLUX
on Ne.
Listed
In some
of the results.
This is close
An
to our other
found in the daytime.
The valws
in Fig. i7.
We do not believe
concerning
possible
that
seasonal
trends.
The failure
many cases
hence
of the method
probably
the flux errors
stem8
of plotting
from
) are larger
Fobs
a number
at night,
W
Ne
of camses
(2) there
!
1<5
to
recover
including:
a
constant
flux F, at night in
( i ) the velocity
is only a limited
errors
height interval
(and
over which
TABLE Vlll
ESTIMATES
Date
(1969)
OF
Nighttime
(EST)
NIGHTTIME
PROTONOSPHERIC
Linear R.nge
F r (el\cm2\sec)
(km)
16-17
January
2200-2330
30-31
January
0130-0230
5-6
February
2330-OIIM
-4X
12-13 February
230Q-01 CO
-5X107
500-70Q
26-27
February
0000 -G200
21-22
March
2300-0100
–9x
500-700
25-26
March’
2300-01
9-10
April
23O+3-O1OO
23-24
April
2230-0030
6-7
MJIy
2230-0030
30-31
May”
1-2
June’
5-6
June*
0100-0200
23-24
June
0100-0200
I-2
July
2330-0030
9-10
July’
220+3-01 00
29-30
July
0000-0130
14-15
August*
2300-0100
9-10
September”
2300-0100
23-24
September
0030-0200
14-15
Octcber’
2300 -OILXI
M
-1.5
XI07
10’
10’
-3.5X107
–4.4x
500-700
700-900
107
+2X107
-1.
lx
-9
lo’
XI06
-2.4x107
600-800
450-700
1
3-4
November
?0-21
November
0030-0230
8-9
December
2300-0130
k Day added.
Upward f! .x!
Poor velocity
profile
Poor velocity
profi 1.
500-900
500-800
500-900
1
-2.4x
Comment
600-9LII
2300-0100
!
FLUX
107
1.9 XI07
500-700
450-704J
—
-,.0
.,.,
—
Q
~,.-7.8—
:
>
: .,.,
5
~
.
~.
.7. * —
\/
2
.
-,,0
—
-,.8
I
!
JAN
,
i
,
““l
with height,
F.
and these
tionary
in those
layer).
arriving
conditions
Figs.
Similarly,
ruary
cover
(w).
VALUE
I
I
,[?
0.,
I
1
.0”
. . .
flux w date for 1969 (Table Vlll).
knowledge
flux is able to balance
of the rate of change
tbe loss,
of vertical
velocity
by night than hy day.
.
-.
that the daytime
where
is not moving
this level
flux is usually
from
near
vertically.
provides
is close
we conclude
estimate
were
obtained
a“terma
the vertical
a sta-
to the value of the
that under equilibrium
of the flux being exchanged
by averaging
those by the density
by about
(indicating
the flux at this height
Fig. 18, as the redwed
to have caused
this level
Thus,
a useful
estimates
fu13y developed
flux is height-independent
we have computed
The actual
has been omitted
escape
the upward
delay and multiplying
(Sec. 11-A) appears
noisy
I
1“,
even when the protono8pheric
Accordingly,
and 5. O-msec
J..
in Fig. i 6 the flux observed
the flux through
4 8(a) through
at 4.5-
arriving
are smaller
cases
flux when the layer
the protonosphere.
J“.
CORRECTED
650 km
It can be seen in Fig. ii
650 km altitude,
I
I
..”
upon an accurate
changes
Flux Through
1P*
Plot of nighttime
depends
I
I
MA.
0+ flux can be expected
and (3) the method
1
I
e,,
17.
Fig.
a steady
OBSERVED
VALUE
0
and plotted
the velocities
at 650 km.
observed
The plot for 26-27
gain brought
drift velocity
with
this in
about
estimates
Feb-
by the snow
to be extremely
and unreliable.
The most
Iisbed
striking
at sunrise
the layer
near
sunset,
may be introduced
of Figs.
the transition
at a time near noon.
of TIDs.
from
Thus,
bution
too late in the day.
was computed
[Fig. ii(j)
exact
flux moved
The sunrise
times,
there
onset
adjusted
ceases
from
by +i4 minutes
fhx
estab of
many of the fluctuations
to downward
fluxes
On some
above
days,
650 km,
an upward
flux is usually
(to allow
ii?
appears
in which the daytime
to be those
to be any escaping
of the upward
While
that a significant
and (r)] appear
to an altitude
1, so that the transition
time at which
These
i i(c)
of the curves.
upward
flux set up by the decay
it is believed
the two cases
[Figs.
downward
component
is real
52
upward
ward at all altitudes
ward to upward
nature
(i) the large
(w) are:
(2) the large
of measurement,
of the presence
On many days,
18(a) through
of the layer,
and (3) the oscillatory
by errors
and a manifestation
sunset
features
by the growth
in which
to occur
flux was found to go downthe vertical
velocity
the height of the transition
e.g.,
9 -iO April
to a downward
well before
[Fig. ii(f)],
flux in Fig.48
from
distridown-
23-24
June
may not mark the
flux.
a readily
recognizable
for the difference
between
feature
local
of the records.
and standard
time),
16-17
JAN 1969
‘t
“’ma.
1
02.0
I
Mcc
I
0600
0s00
I
IOm
!
,200
1
)...
1(
1,.,
),..
1
zoo.
1
=w
2*
EST
(.)
SUNSET
SUNRISE
.4 —
-,
,m
&
&
&
JOO
,:00
,,100
,,’00
,6’00
,,00
I
,
,00,
,,.0
,4C+
Esl
[b)
Fig. 18(a-w).
in Table V1.
Values
of log Io (F)65o,
i.e.,
These are thought to be cl-e
i48
—
flux through 650 km for the days listed
to actual
pr.ionospheric
flux.
,
~16-2-11M&-11
P-IQ.
,
0
w
SUNRISE
SUNSET
-4 –
-,
mm
,2100
MOO
I
.600
08W
1oOO
,2..
1400
1600
18W
2000
“0°
“m
EST
(c)
2
~
12-13
FEE !969
o
00
;
>=
~
-,
~.
o
=,
~
.
,SUNSET
S“NRISE
- ,–
- , \,oo
Im
,4,.
\
C6m
I
.,.0
,
Wca
,.00
I
14C0
EST
(.51
Fig. 18(.a-w).
ii9
I
A
1
Continued.
,
~600
1
1,,,
1
,000
,
2,00
MC.?
~
3 –
25-26
MAR ,96,
* -
;0
.\~
<
,
~, .,
~
;
> -* —
:
-3 —
.4 -
s“.,,,.
-, SUNSET
I
“’o OCO 0,00
1 1111[11,
0400
.,0.
t,
08.0
,000
,,0,
Fig. 18(cJ-w).
420
Moo
Continued.
),00
,800
moo
,*C-O
,,(
EST
[g)
-*
‘1
t
-,
,Wo
&
&
1,,1
SUNSET
SUNRISE
-, -
I
0600
1
CSC4
,
1000
I
!200
Fig. 18(0-w).
,
1400,
Continued.
121
1600
I
,,~
zooO
2200
2w0
0)’ \
\
-3
-4
1
SUNSET
SUNRISE
-5 -
t
-e
C@.
O*OO
I,llljsl
Mm
C6ua
O*W
1000
,.~
,.~
1,..
l...
,-
2=-3
2+,
EST
(1)
00
-8
.OOO
I
,,@
I
.400
I
06o0
0800
I
IO..
IZGO
,
IMCU
EST
(1)
Fig. 18(0-w).
$22
Continued.
I,..
IWX
ZW5
Z*
z40
1
‘~\r
0
.1
-2
.3
SUNSET
‘U NRISE
t
I O*CO
-50000
I
0.00
,
I
060,
,,0,
,
)00.
,,..
,4.0
,.00
,800
,.0.
,x.1
,4(
EST
(k]
2—
23-24
JUN 1969
fiu
Q.
A
.<
< iv
-z -,g
5 .,—
~
-3 —
SUNSET
-+ -
‘ 0000
‘“’’’’”
,
0200
t
0400
I
0,00
I
.,00
I
!0.0
I
)200
I
1400
Es,
{11
Fig. 18(a-w).
323
Continued.
I
1600
1
leoo
1
200
t
I
2200
2.0
,
,8-2-1)98!
+
],8-2 .11838-11
39-1o
duL
1,69
1-
0
73
.<
<.
w
,
“2
1
>
“- ,3-
s“NRISE
4-
‘0000020.
1,
Moo
0600
0,,
EST
(n]
Fig. 18(a-w).
Continued.
i24
29-30
d“,
1969
2 -
;0
:
,5
.
-f
“g
;
.
#
.?
0
-3-
S“N.ISE
..
-,
Ocoo
,
0200
II
0400
\
0600
!
,*OO
I
,,.0
,,00
1
,.00
,
,,,0
(
!8,0
1 I
,,00
,,00
240,
EsT
.4
–
SUNSET
SWR(SE
-5
0
-’0000
0200
,
..00
.,00
,
moo
,
,,0,
I
,.00
,,0,
EST
{P]
Fig. 18(a-w).
125
Continued.
1
(,,0
I
,,00
moo
1
,200
MC
-5
m+.
ozoo
1!
..00
$
I
0600
.s00
400.
IZOO
I~o.
f,..
1
t,..
II
2000
I
2,00
I
2+~
EST
(q)
-4
t
‘t‘u”’”
ISUNR”E
Fig. 18(0-w).
C.ntinued.
126
23-24
-mm.
SEP !9s9
3 -
, —
{
.;
o
{
., _
..
:
-2 —
.3
..
-’0000
moo
0.00
06,,
mm
’000
,,00
,4.0
,,.0
,,,0
moo
2200
2.00
EST
(s)
,
-,
t
-.
SUNSET
SUNRISE
-,
0...
1
.2.0
I
0400
0600
,
0800
{000
,
!200
I
!.00
EST
(I1
Fig. 18(a-w).
Cc.ntinued.
1
,600
I
,.00
I
2..0
1
2200
Z400
3-4
NOV 4969
#
~
o
-, –
0
-z –
o
0
-3 –
.4 -
-,
–
I
“’0.00
.20.
0400
,
0600
0800
1000
,
IZOO
I
f400
ES,
(.)
,
,,
[“1
(
Fig. 18(a-w).
i28
!,
—
Continued.
I
1600
(
1800
2000
2200
‘“w
I
8-9
DEC 4969
I
i
1
-.
-,
,0000
I,I((IIILI
SUNSET
SUNRISE
0200
0.00
0600
on..
,000
s,..
,4..
s...
~,oo
*000
=oo
2“00
EsT
(.)
Hg.
are
plotted
at o,
in Fig.
%00, 200,
time coincides
rise
and sunset
observed
before
Ccmtin.ed.
they are superimposed
on curves
and 300 km (Ref. 59) for 4Z” latitude.
closely
times
at sunset
the 200-km
Fig. 19.
i 9 where
18(.-w).
with the time of sunrise
have been indicated
usually
begins
sunset.
The onset
It is clear
prior
It is striking
to the sunset
of this downward
the times
of sunrise
fFOm tMs PlOt that the Onset
at 200 km altitude.
in Fig. i 8.
1 to 3 hours
indicating
Accordingly,
that the large
time and peaks
flu% is thought to be caused
tbe 200-km
downward
flux
at or slightly
by tbe decay
Times of onset of upward flux (F;g. 18) compared with sunrise in ionosphere at different
i29
sun-
altitudes.
of
the F -laj-er
during
to a thermal
collapse
the downward
Large
At sunset,
the temperature
Sometime
the two effects
30
of the layer.
in the downward
nights,
that could
open the source
decreases,
to give separate
leading
peaks
in
give rise
flux (e. g.,
to the observed
rising
increases
to 5 X i08 el/cmz/see)
during winter
36
in Nina,
do not appear to occur,
thus
of this ionization.
SUMMARY
Incoherent
vertical
scatter
velocity
data on F-region
have been
gathered
(42. 60N, 7 i. 50W) approximately
the altitude
density
interval
(near
a complete
modes
profile
report.
Contour
density
summer
year,
of April
were
and stationary
(Table
flux for these
By assuming
flux profile
was filled
to identify
times.
motions
could be obtained,
From
be 500 el/cm3/sec.
in the data,
it is difficult
and/or
were
observed
and ion temwinter
the beginning
and
of the
encountered
during
the
and the valley
region
be-
curves
showing
instrumental
the production
200 km altitude
noon when the layer
flux that would account
The flux through
begins
for the winter
the altitude
obtained
variation
in the results
were present.
about 700 km,
a corrected
flux appears
to be 5 X
rate at 300 km was deduced
flux at all
altitudes
Owing to the greater
flux,
but the best
tbe level
sunrise.
increases
with a
appears
that large
Downward
Large
to
uncertainties
estimate
650 km 8hows
until late at night.
nighttime
of
near noon suggests
above
ionospheric
to decay
appeared
biases
show a downward
the true protonospheric
flux.
when the F-layer
value for the escaping
flux,
flux curves
soon after
of the downward
(z)],
a characteristic
precipitation
near the peak of the layer.
upward
after
have been described
7(a) through
exhibits
of many of the curves
and an average
to establish
are established
for
vs height and time of electron
be altitude-independent
the downward-going
escape
fluxes
of i 5 km in electron
methods
near noon and midnight
layer
flux should
to be half that for the daytime
for a period
span
The time resolution
the two (in 1969) around
and have constructed
magnitode)
The results
upon which of two operating
Te [Figs.
were
and
Hill radar
in.
The character
The nighttime
peak (of very uncertaim
II).
parameters.
density
temperatures
periods
of the entire
that the escape
107 el/cm2/sec.
VI),
(Table
depending
temperature
of auroral
electron
i969
the variation
between
and ion temperatures,
at a time at the Millstone
and reduction
The electron
Two cases
high F-region
We have attempted
that significant
showing
with a rapid transition
tween the E- and F-regions
stable
30 or 45 minutes,
electron
(z)].
electron
with a height resolution
The data-collection
(z)],
8(a) through
and October.
when very
vertical
approximately,
and 75 km in the other
cons tructed
3(a) through
Ti [ Figs.
behavior
months
V).
densities,
of 24 hours
per month throughout
was either
(Table
20
diagrams
&,e [Figs.
perature
twice
200 to 900 km,
altitude
electron
for periods
the peak of the layer)
was employed
in a previous
exist
of the p3asma
appear
flux.
increases
leaving
Vf.
30
the afternoon.
fluxes
increases
of the F-layer
were
not seen.
*3O
,j
—
,.—.......___
.._..
______
z__=_.=.
j_
,
APPENDIX
I. INTRODUCTION
It is possible
produce
Figure
bya
A-i
cathode
impinges
by field
to calculate
from
first
dinthe LIHF transmitter.
shows
a section
is accelerated
on a grounded
coils
around
with distance
through
through
The beam
the klystron.
alongtbe
amplifier.
Vvolts
value of the frequency
Abeam
of electrons
and then traverses
of the beam
magnetic
is modula.ted
RF field
field
produced
by the RF fieJd across
in the beam
can be excited
HEATER
SUPPLY
giv.m off
a drift tube until it
by an axial
of ‘nbunchingrt of the electrons
so that a much larger
offset
the method,
is kept in focus
Tbe velocity
The degree
beam
the approximate
outline8
tbe klystron
a potential
collector.
tbe gap in the input cavity.
principles
This Appendix
across
increases
the -P
in the
~
CATHODE
I
.
I
INPuT
cOAxlAL
m
.P.TCA=
1-
]
“y”e
m
‘L=”
““cl JEl=”’’’””””’
WATERCOOLED
COLLECTOR
Fig. A-l.
output cavity,
the energy
being
,
wed
I
up heating
the water that cools
and hence
the efficiency
H.
at Millstone,
gained
at the exptmse
of the beam
the collector.
.mplifiertuhe.
of the energy
energy
) The idler
in the beam.
is extracted
cavity
serves
(In the klystrons
and the remainder
to improve
ends
the bunching
of the device.
PHASE SHIFT fN THE
KLYSTRON
r required
output CaVitie S introduces
I
Cross section ofklystron
only about 30 percent
The time interval
v
a fixed
for the electrons
phase
difference
to traverse
q between
the distance
d between
input and
tbe input and output signals.
Hence
q =2rfr
where
f is the radar
frequency
r = d/ve
where
a voltage
(440 MHz).
The time interval
T is given by
(A-2)
sec
Ve is the electron
through
(A-1)
rad
Vle can compute
~elocity.
Ve knowing
that the electron
has fallen
V from
electron
energy
. i/2
me(ve)z
. eV
(A-3)
Combining
Eqs. (A-i),
(A-2),
and (A-3),
we have
_-
~.
Scaling
the
drawing
and rn:
= 9.108
JL ‘ad
2rfd
%
of tbe x626Ac
x 10-28
(A-4)
~
we find
klystron,
d = i08 cm.
Since
i eV = i.60
X iO
-iz
ergs
g, we have
(A-5)
where
lfI.
V is the klystron
VOLTAGE
Although
DROP
voltage.
DURING
the current
voltage
drop occurring
change
of applied
THE
I through
during
voltage
PULSE
the klystron
a pulse,
varies
we may assume
with the applied
voltage
that it is constant.
V, for the small
Hence,
the rate of
is
(A-6)
I
Here,
C is the capacity
fa13 in voltage
[from
during
Eq. (A-5)]
,:
FREQUENCY
A constant
tbe pulse
causes
bank (24 #F) and I is the current
the phase
shift
q during
the pulse
during
to change
a pulse.
The
at a rate given
in
~
IV.
of the condenser
❑ –2n
80i.7
~
$
rad/sec
of the phase
difference
(A-7)
.
SHIFT
rate of change
mm-responds
to a frequency
shift Af that is
given by
Af=;r~
~Z
~.~
2
V312
(A-8)
.~Hz.
432
8ubstitutimg
for dV/dt
[Eq. (A-6)],
~f . -400.81
~$/2
-1.67
we obtain
~z
X i07 1 Hz
v3/2
(A-9)
V. CURRENT READING
AS shown in Fig. A-2,
only the average
Fig. A-3(a)
current
where
the current
Iav.
t represents
through
The actual
the klystrons
current
the interpulse
waveform
period
is read by a meter
through
(i3. O msec
for B-mode,
which measures.
is shown-in
20.0 msec
for
1
1
KLYSTRON
HIGH-
the meter
KLYSTRON
4
2
I
I
VOLTAGE
POWER
SUPPLY
+
Fig .A-2.
DkJgr.am of power supply cmtpnents.
II
I
I
Fig. A-3.
C-mode)
Waveforms
for current
and T is the modulator
age and peak currents
I=FI
are related
I
(b)
pulse
and VOI toge applied
length
(i.0
msec
to klystrms:
(~) current,
for C-mode).
(b) v.dt~ge.
It is clear
that the aveI..
through
(A-io)
av
133
1
where
F is a duty factor
in the B-mode
to keep the average
T = 0.61 msec.
Thus,
the frequency
B-,
–4.67
VOLTAGE
a modulator
pulse
length
C-mode
(A-ii)
.
X i07 F1av
(A-i2)
~3/2
READING
The voltmeter
employed
waveform
voltage
This requires
constant.
length is adjusted
shift may be written
M.
VI.
current
pulse
Thus,
F .18.0
(
The modulator
equal to i 8.0 in the C-mode.
to measure
of the form
there will be a voltage
the voltage
applied
As current
shown in Fig. A-3(b).
drop through
to the klystron
the tivo resistors
(Fig. A-2)
is drawn through
that connect
will havea
the klystron,
the klystrons
to the condenser
bank of
AVi =22.5
There
will bea
further
~v
2
FIav
voltage
. <v XT
dt
FIav
—
24 X 10”6
At the end of the pulse,
This will recover
with a time
volts
drop during
the pulse
of
~olt~
volts
the voltmeter
to its former
(A-43)
.
.
(A-i4)
will agati
see the fu13 voltage
value as it is charged
through
applied
to the condenser
the 65- and 6.25 -ohm
C.
resistors
constant
~= (65 + 6.25) C
.i.71xi0-3
Thus,
the voltmeter
reads
sec
a value
(A-i5)
.
Vm which is less
than the voltage
V! on the condenser
bank
by an amount
l’! –Vm
= ~ IavF [22.5 (T+
10-4)
+ 2.o8 X iO T(T+
i.71
X iO-3)]
.
(A-i6)
Hence,
VI - (vm)B
.3.49
IavF = 62.9
V1 – (Vm)c
= 4.05
IavF = 72.9 Iav
The voltage
bank
V applied
to the klystrons
$v
V01t5
Volts
during
(A-i7a)
.
the pulse
V 1 by an amount
●
i 34
(A-i7b)
is also
less
than that on the condenser
AV2
V! -V=AVi
+ ~
= FIav[Z2.5
Vi – VB = 633 Iav
volts
VI - Vc = 779 la”
volts
It follows
that,
during
the meter
less
-5701
the pulse,
~v volts
+2.08
X 404T]
(A-18)
(A-i9a)
.
(A-i9b)
the voltage
applied
for the B-mode
to the klystrons
and -700
Iav volts
will be the amount
in C-mode.
given on
ThUS, Eq. (A-i3)
may be written
3 x ios
Iav
AfB =
(A-20a)
(Vm -570
3x4081
AfC
=
(Vm
The corresponding
velocity
-700
errors
I
av
)siz
av
‘z
Hz
.
(A-20b)
Iav)3/2
Aw are
ios 1=”
m/s
‘WB
= -
(Vm -570
io*
‘Wc
= -
ec
(A-21a)
m/s ec
(A-2ib)
1=”)3/2
Iav
(Vm – 700 ,Iav)3/2
135
A~KNOWLECGMENTS
The aufbor is grateful to W. A. Reid, J. H. McNaIly, L. B. Hanson, and others
of tie staff of Millstone Hill who gathered data reported here.
R. F. Julian and
J. K. Upham were responsible
for writing the computer
programs
required to
process
the data, while Mrs. A. Freeman
a“d Mrs. J. LaJoie carried out the
work of plotting graphs and performing
some calculations
by hand.
During
1969, the incoherent
scatter
work at Millstone Hill was supported hy the U.S.
Air Force through its program of general research
at Lincoln Laboratory.
REFERENCES
1.
J. V. Evans,
Reoort 374,
, “Millstone Hill Thomson Staffer Remits for 1964: Technical
Laboratory,
M. I. T. (15 November 1967), DDC AD-668436.
Report
430,
Lincoln
, “Millstone Hill Thomson Scafter Resdts
for 1965: Technical
Laboratory,
M. L T. *8 December
1969), DDC AD-707501.
Report
474,
Lincoln
, “Millstone HOI Thomson
Laboratory,
M. L T.
Report
481 I
Lincoln
“Millstone Hill Thomson Staffer Results for 1967;
L&oratory,
M. 1. T. (22 July 1971), DCC AD-735727.
Technical
Report
482,
Lincoln
, “Millstone Hill Thomsm Starter Results for 1963: Technical
Laboratory,
M. L T. (23 ]amary
1973), DDC AD-767251/2.
Report
499,
Lincoln
2.
3.
4.
5.
6.
, Planet.
7.
8.
“Ionospheric
%.ckscatfer
Observations
at Millstone Hill: Technical
Lincoln Laboratory,
M. I. T. (22 January 1965), DDC AD-616607.
Space Sci.
. ]. Geopbys.
—
Res.
1175 (1965),
9.
, Ptanet.
Space Sci.
g,
, Planet.
Space Sci.
M,
11.
, J. Atmos.
, J. Geophys.
12.
Results for 1966: Technical
, DDC AD-725742.
L3, 1031 (1965),
~,
10.
Terr.
Staffer
EIys.
DDC AD-616607.
DDC AD-61431O.
1387 (1967).
1225 (1970),
Z,
DDC AD-716056.
1629 (1970),
DDC AD-716057.
Re.s. 7&, 4803 and 4815 (1970),
DDC AD-714447
and AD-714446,
respectively.
13.
, Planet.
14.
, J. Atmo..
Space Sci. z,
Terr.
and I.J. Gasfman,
15.
763 (1973).
S%YS. %,
J. Geophys.
Res.
16.
R. J. Cicero”e and S. A. SowhiU, Radio Sci. 6,
partment
of Electrical
Engineering,
University
17.
J.V. Evans
and L. P. Cox, J. Geophys.
18. L. P. Cox and J.V. Evans,
19. J.V.
20.
Evans,
j. Geophys.
J. Geophys.
Res.
DDC AD-772 ~3716.
593 (1973),
DDC AD-77 ~877/8.
25, 807 (1970).
159 (1970),
Res.
X,
Res.
Z5, 6271 (1970,
17, 2341 (1972),
DDC AD-704626.
957 (1971) [ahm Aeronomy Repofl 39. Deof Illinois,
Urbana (1 September
1970)1.
DDC AD-703492.
DDC AD-722911.
DDC AD-752948.
Scatter Measurements
, R. F. Julian and W.A. Reid, “Incoherent
Censity, Temperatures,
and Verticat Velocity at Millstone Hill: Technical
Lincoln Laboratory,
M. L T. (6 February
1970), DDC AD-706863.
21.
J. P. McClure,
H.C. Carlson,
(1973).
22.
J. E. Salab,
PhD Thesis,
23.
A. E. Hedin, H.G. Mayr,
Res. 29, 215 (1974).
of F-Region
Report 447?
W. B. Hanson, A. F. NagJ, R.]. Cicerone,
L. H. Brace, M. E&on, P. L!a.er,
J.V. Eva”s, G.N. Taylor and R. F. Wocdman, J. Geophys. Res. 18. 197
“A Study of the Midlatitude
Meteorology
Department,
C.A.
Reber,
Thermosphere
by Incoherent
M. I. T. (Augwst 1972).
N. W. Spencer
i 36
Scatfer
and G. R. Carignan,
Radar f
J. Geophys.
y77
—
!
24.
H. G. Mayr and H. Volland,
J. Geophys.
Res.
25.
D. Alcayde,
26.
J. E. ?.alah, J. V. Evans and R. H. Wand,
27.
K.L.
28.
P. E!auer and J. Fontanari,
Jones,
29.
—!
T. Tamka
30.
J.V.
J. Atmos.
Terr.
Phys.
Radio
SCL
31.
ibid
, _.,
32.
, J. Geophys.
6
_.
843 (1971),
R...
Res. 29,
629 (1974).
Radio Sci. ~, 231 (1974),
N,
DDC AD-785097/7.
1311 (1971).
609 (1971),
6,
6774 (1972).
J. Geophys.
ibid
35 1515 (1973).
_.!
.$
and K. Hirao, J. Atmos. Terr.
Evans,
27,
Phys. N,
1443 (1973).
DDC AD-731927.
DDC AD-737929.
~,
4331 (1965),
DDC AD-623606.
33.
U.S. Department of Commerce, Envirrmmerdal services Administration,
- ITS Ionospheric
Predictions for January 1969,” TB 11-499-70/TO
31-3 -28-2 (October 196 B).
34.
J. A. Klobuchar,
J. Aaronsand
H. H. Hoseinieh,
35.
J. V. Evans,
36.
A. V, Mikhaylov,
37.
W. B. Hanson and T. N. L. Patterson,
38.
T. Yonezawa,
J. Geophys.
Res.
Geomag.
~,
J. Geophys.
3489(1968),
and Aeron.
M,
Res.
Planet.
DDCAD-673605.
Space Sci. U,
979(1964).
39.
40.
J. E. Geisler,
Res.7Z,
7530(1968).
653,(1972).
Space Research V, 49(1965).
———
l. E. Geisler and S. A. Bmvhill, Aero”omy Report5,
Department
ing, Uniyersityof
Illinois,
Urbana (l January 1965).
J. Geophys.
X,
of Electrical
En@neer-
81(1967).
41.
V. A. Vasin,
42.
G. S. Ivanov-~olodnyy
and A. V. MikbaylOv,
43.
H. Risbbetb,
Terr.
44.
P. Y. S. Hsuand S.F. Chii, “Mahttemnceof
Nighttime F-Region:
Observadonof
8pheric Eledro” Flmat&ecti,”
J. Atmos. Terr. Phys. (Lu press, 1975).
L. V. Grishkevich
J. Atmos.
45.
R. Rtister, J. Atmos. Terr.
46.
T. E. VanZandt,
and V. V. Pisareva,
Phys. ~,
Pbys.
V. L. Peterson
47.
C. G. Park,
48.
C. G. Park and C. LMeng,
J. Geophys.
49.
J. E. %.lah and J. V. E“ans,
50.
G. Lejeune
and G.N.
Res.
a,
El,
473(1970).
N, 39(1973).
Exo-
765(1969).
J. Geophy.s. Res.
z,
27 S(1971).
4650(1971).
J. Geophys.
Res.
Space Research
Taylor,
and Aeron.
and Aeron.
1(1972).
and A. R. Laird,
~,
Geomag.
Geomag.
Planet.
Z@, 8326(1971);
also seelg,
XIII (.Lkademie-Verlag,
Space SCL ~,
3B28 (1973).
Berlin,
1973). P. 267.
1061 (1972).
51.
[. V. Evans,
52.
1.V. Evans, R. A. Brockehnan,
R. F. Julia”,
Sci. 5, 27 (1970), DDC AD-704631.
53.
[.V. Evans and J. M. Holt,
54.
V. W.J. H. Kirchoff and L. A. Carpenter,
“Dominance of the Dimmtd Mcde of Horizontal
Jrift Velocities
at F-Region Heights:
J. Atmos. Terr. Phys. (in press,
1975).
55.
{. W. Schunk and J. C.G.
56.
‘. E. 3aLah and J. M. HoIt,
57.
‘.L. Massa
58.
L Risbbetb and O.K. Garriott,
iew York, 1969), pp. 170-171.
59.
. . Colin and M. A. Myers,
“Computed Times of Smrise
L4.SA Technical Memor.md”rn
TM X-1233 (April 1966).
J. Geophys.
(private
Res.
~,
2344 (1973),
DDC AD-772214/3.
W. A. Reid and L. A. Carpenter,
Radio Sci. ~, 855 (1971),
Watker,
Planet.
DDC AD-738727.
Space Sci. k,
Radio Sci. ~, 301 (1974),
Radio
855 (1971).
DDC AD-7 B5096.
communication).
Introduction
to Ionospheric
Physics
and Sunset
(Academic
FTeSS,
in the Ionosphere
,“
i 37
———.
UNCLASSIFIED
En,
,. . .. <,,.,,-..!..
.. . . . “,
. 7., s. ,.,. .-,. ,uf,,... D.,.
——.
.—
...
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REPORT
e,ed)
READ 1NSTRUCTIONS
PAGE
BEFORE COMPLETING FORM
2. GOVT ACCESSIONNO. 3. RECIPIENTS CATALOGNUMBER
DOCUMENTATION
1. ,6?ORT .UM8ER
ESD-TR-74-234
5. TYPE OF REPORT & PERIOD COVERED
i. TITLE !.mi S.h!itte)
Tecknical
Millstone
Hill Thomson
Scatter
Results
6.
PERFORMING
ORG.
Technical
7.
AU THOR(,
8.
I
Evans,
9.
0RGAN12AT10N
Box
REPORT
NUMBER
Report
OR GRANT
513
NUMBER(S)
F1962 8-73-C-0002
NAME
Lincoln Laboratory,
P. O.
CONTRACT
John V.
PERFORMING
Report
for 1969
AND
10.
ADDREs5
PROGRAM
ELEMENT,
AREA & WORK UNIT
.
PROJECT,
NUMBERS
TASK
M. I. T.
73
7X263304D215
Lexington, MA 02173
11.
CONTROLLING
OFFICE
NAME
AND
12.
ADDRESS
Sallistic Missile Defense Program Office
Department of fhe Army
1320 Wilsm Poulevard
Arlin@on,
VA 22209
14. W3NITOR,NG AGENCY NAME & ADDRESS (({ difie.enl /,0”!
DISTRIBUTION
STATEMENT
Approved
(oj,his
13.
18.
S“PF’LEMENT.4RY
NUM8EROF
PAGES
144
15.
CO”1,0111T8 o!{i.d
SECURITY
Uncla
15.I.
CLASS.
(./
thi,
w@)
sified
DECLASSIFICATION
5CH EDULE
DOWNGRADING
Re.wrt)
for public release;
!7. US7R[BUTION
s~~i’~.$!mi~(.[
DATE
23 ]Ldy 1974
Electronic
Systems Division
Hanscom Air Force Sase
Sedford, MA 01731
16.
REPORT
the
distrfbutim
nbstrcact
entered
unlimited.
in Block
20,
i{ di,ffemnt
jr.”!
Report)
NOTES
Nom
19,
K E“
WORDS
(Cm,;,,”<
on ,.”.,s.
,(d<
;( ,,ace,
smy
and
”..
on ,,”,,s.
67 block
number)
electron den sity
ionospheric
scatter
sea sons 1 variations
Millstone radar
F-region
diurnal variations
!0. ABSTR~C7(Co”,,
ide,,tijy
s,de
;/ ,w<e,
sa.y
.md
;dent,/y
by Mock
temperature
effecfs
spectrum analyzers
“u”Ib8r/
report summarizes
the results for the electron density distribution,
elecfron and ion temperatures
This
and vertical ionization fluxes in tbe F-regim
obtained during 1969 using the Millstone Hill (42. 6“ N, 71. 5“ W)
These data, for tie hei$m interval approxim.cely
200 to 900 km
Them.sm (incoherent)
scatter radar system.
were @bered
. . . . 24-hour observing periods,
roughly twice per calendar month.
The time resolution
to
obtain rcmlts
over this emire height imerval was eifher 30 or 45 minutes,
depending upon which of two operating modes was employed.
The results for the diurnal variation of fhe electron demity and temperature
exhibit the characteristic
summer and winter p.mterm discussed
previously.
The transition
he fwee” the two takes pbCe in April and
. .
,“. ”
LJD , ;;N;3
1473
EOITION
OF
1 NOV
65
15 OBSOLETE
UNCLASSIFIED
SECURITY CLAs51FficAT10NOF rH15 PAGE
(when
O.,O
Kn,e,
<d)
4
20.
(continued)
October,
TWO cases of overhead auroral precipitation
were observed
efforts to observe a stable red arc.
Other instances
of geomagnetkally
1
during the year as a consequence
of
disturbed behavior were infrequent.
Vertical fluxes of ionization were measured,
and the flux escaping to the magnetosphere
near midday
was found to have an averap
value of -5 x 107 el/cm2/.sec.
NW midrd$n,
the magnetosphere
appears to
~PPIY tie 10~1 iOnOs@ere witi a flux of atmtt half ttds ~O~t.
{
i39
* “. ,. .0,,,..,.,
mrm,ws
owl.,:
,975 --60, -,,,..,,