Technicd Report
530
J. V. Evans
Je M. Halt
Millstone Hill
Thomson Scatter Results
for 1972
18 September 1978
Prepared for the National Science Foundatiou
under NSF Grant No. ATM 75-22193
Lincoln Laboratory
MASSACHUSETTS INSTITUTE OF TECHNOLOGY
ABSTRACT
During 1972, the vertically
(42.6”N,
directed incoherent scatter radar at Millstone Hitt
71.5“W) was employed to measure electron
temperatures,
and vertical ion velocity
one or two times per month.
900 km, approximately,
in tie F-region
density,
electron and ion
over periods of 24 hours,
The observations spanned the height interval 200 to
and achieved a time resolution of about 30 minutes.
This
report presents the results of these measurements fn a set of contour diagrams.
For a number of the days, the spectra of the signals gathered at altitudes between
450 and 1125 km have been the subject of furfher .malyeis in an effort to determine
the percentage of H+ ions present over Millstone.
ions are escaping from tbe F-region
The results
suggest that H+
to the magnetosphere m a value close to the
theoretical limiting flux during the daytime in all seasons.
comes downward commencing neax midnight in winter,
At night the ftux be-
but may rem afn upward
throughout the night fn summer.
iii
.—. _..__.,..
-...,—
cONTENTS
iii
Abstract
1.
11,
EQUIPMENT,
PROCEDURES
A.
i.
B.
,
v.
DATA-ANALYSIS
2
General
New Ionosonde
:
8
Procedures
9
Data Reduction
RESULTS
FOR ELECTRON
DENSITY,
ION TEMPERATURES,
AND VERTICAL
ELECTRON
VELOCITY
AND
+3
General
i3
B.
Quiet Winter
96
C.
Disturbed
D.
Quiet Summer
E.
Disturbed
A.
i
AND
2
Observing
c.
Iv.
OBSERVING,
Equipment
2.
111.
1
INTRODUCTION
RESULTS
Behavior
Winter
Summer
FOR
96
Behavior
97
Behavior
99
Behavior
H+ DENsITIES
AND
99
FLUXES
A.
General
99
B.
Data Reduction
99
C.
Accuracy
103
D.
Results
403
E.
H+ Concentration
F.
H+ Fluxes
DISCUSSION OF
AND FLUXES
A.
Comparison
B.
Control
C.
Comparison
107
Profiles
Mo
THE
RESULTS
with Previous
of the Diurnal
FOR
H+ DENSITIES
Experimental
ill
141
Findings
143
Variations
with Theoretical
116
Models
Acknowledgments
il?
References
417
APPENDIX
– INSCON
%21
Summary
v
.
MILLSTONE
1.
HILL
THOMSON
SCATTER
RESULTS
FOR
1972
INTRODUCTION
Since
‘1963, incoherent
densities,
and electron
Massachusetts
reports,
obtained
(4Z.6” N, 7i.5°W)
and presents
observations
reported
in earlier
transmitted
(Thomson)
scatter
and ion temperatures
were
years
to the World
gathered
in this program
made for periods
of 24 hours,
have been published
Data Center
A,
(68-cm
Year
February
1963
March,
April,
UHF
August,
September
November
ReF. t I
Ref.2
November
April,
Ref.10
Ref.12
Ref.3
Ref.13
August
Ref.14
August,
March,
Ref.4
December
July,
Septemb=r
June,
Oc+ober,
through December
R.4.16
Ref.5
through December
Februory,
January
Ref.15
Septembsr
thrwgh
January,
January
December
Ref.16
Ref.6
Ref. 17
October
Jmwarythrough
1969
HILL
RESULTS
Ref. 1
through December
January
1968
SCATTER
June
June,
1967
MILLSTONE
1963 to J.n..ryl964
July,
January,
1966
THE
through December
Ja.wry
1965
I
THOMSON
February,
April,
September,
December
July
October
i972.
Ref.7
Ref.18
Ref.19
1970
January
through December
Ref.8
1971
January
through December
Ref.9
The
The results
I, and have been
Publication
July,
January
I 964
in Table
West ford,
of annual
year
a month.
Months Covered
July,
April,
a series
during the calendar
listed
electron
Hill,
Colorado.
CONCERNING
Wavelength)
of F-region
at Millstone
once or twice
in the articles
Boulder,
TABLE
PUBLICATIONS
measurements
This priper is the tenthin
(Refs. i to 9).
the results
radar
have been conducted
The
results
reported
ion temperatures
900 km,
in this paper
Te and Ti,
approximately.
are
and vertical
of F-region
velocity
The measurements
were
ments were
be varied
made of the E- and F-regions
allowing
has been described
this pulse -pair
for the digital
in detail
in a number
Other observations
rocket
from
Wallops
(e. g.,
gathered
Island.
In addition,
as part of a program
on
Spectral
whose spacing
could
This
Zi
and
distant hills,
from
ion temperature
in the study of tides in the lower
using
thermo-
Ref. 23).
here include
pass of a satellite
studies
short observing
(ISIS 11) or with the launch of a
some data gathered
of propagation
long pulses
in the computer.
for E-region
in ‘t972 that are not reported
with thq overhead
and
200 to
computer.
of pulses,
of unwanted returns
Results
of papers
conducted
chosen to coincide
12 hours)
sub$ctim
pairs
to he determined
method in 1972 have been employed
and reported
periods
function
elsewhere.
single
in a digital
electron
by examining the outputs from
20
Additional measure (0,5 or i.O msec).
by transmitting
the echo autocorrelation
Net
interval
was obtained
matched to the length of the pulse
apprOach also allowed
sphere
the returns
(from which Te and Ti m-e determined)
a bank of filters
density
made by transmitting
each sweep of the radar time base and integrating
information
electron
V= and span the altitude
over
short periods
have been omitted
(less
than
as contributing
little
to the report.
Section 11 describes
1972, these were
Results
tbe equipment,
changed little
for electron
density,
from
11.
EQUIPMENT,
A.
the previous
procedures.
year
During
and described
and vertical
velocity
for the abundance of H+ ions over
these
results
in Iigbt Of Present
in Ref. 9.
are preMillstone
understanding
and magnetosphere.
OBSERVING,’~ti
DATA-ANALYSIS
PROCEDURES
Equipment
i.
General
The UHF (68-cm
system
employs
dures were
wavelength)
component
simultaneously.
lengths
(0.5,
1.00r2.0
an imperfect
This scheme
msec)
match between
pulses),
some systematic
altitudes
and empirical
tbe filter
errors
were
correction
bank system
steerable
system
is described
timing
was assumed
and the 30-MHz
UHF receiver,
allowed
introduced
to the data-taking
spectra
described
by a digital
observations
L-band
When used for incoherent
scatter
timing
receiver
and sampling
the elements
in Ref. 20.)
2
to remedy
wavelength)
studies,
procedure
some
7,9
this problem.
radar.
control
in the Ionosphere
to the 30-MHz
remained
these.
using the smaller
(23-cm
unit (located
of the filter
of Te and Ti over
scatter
was connected
Owing tO
for the 0,5-msec
which obviated
conducted
for many
Ref. 20.
(especially
in an effort
correlator
were
proce-
for each of the pulse
indetailin
of the pulses
developed
to remeasured
filters
in the measurements
were
This
antenna and hence can measure
the echo power
andhasbeen
scatter
data-taking
to rearrange
has been described.i
modifications
and the spectra
was replaced
by the incoherent
sothatthe
it was necessary
Extensive
procedures
IF output of the L-band
equipment
220-foot-diameter
antenna and aeeociated
in Ref. 24.
radar
made use of banks of matched
employed,
the filters
1972, some incoherent
84-foot-diameter
as described
directed
scatter
of the ion drift.
made in %968 (Ref. 6)wbich
heights
During
incoherent
a fixed vertically
only the vertical
In i976,
results
and discuss
linking the ionosphere
and reduction
and ion temperatures,
we present
in the upper part of the F2 -region
of the fluxes
those employed
electron
sented in Sec. 111. In Sec. IV,
data gathering,
This
of tbe radar
Laboratory)
IF input to the
unchanged.
bank to span a wider
frequency
(Actually,
range
2.
New Ionosonde
The principal
search
ionosonde
nological
vides
fier
change in 1972 to the apparatus
was the introduction
was replaced
Institute
by a !tDigisonde
Research
Foundation
only about 80 mW of RF power,
to be used with it.
on hand.
The original
C-4 sounder
The Digisonde
radar
This transmitter
transmitter
over
coaxial
attenuation
filters
unit, constructed
unit is located
cable from
to compensate
new system
(Fig. 1).
signal
from
the spare
in the building
cables,
broadband
for the attenuation
Together
power
with complete
1 km away.
response
solid-state
until
at the main
via coaxial
signal
(at RF)
To overcome
together
by
the two.
is shown in Fig. 2.
are employed
and tbe printer,
it between
it is located
The received
just over
ampli-
was accomplished
amplifier
C-4 components,
preamplifiers
power
Techpro-
C-4 sounder that was
as a standby system
Unlike the C-4,
vs frequency
of the tape recorder
a transmitter
of a spare
of the c-4
near the antenna.
re-
the C-4
manufactured by Lowell
25
Since this instrument
and switching
to the transmitter
the antenna to the receiver
in the coaxial
With the exception
Standby operation
for both systems
for ionospheric
In February,
to construct
using portions
is shown in Fig. i.
the exciter
sounder
was left intact and available
amplifier
128 sounder
site and supplies
sounder.
Massachusetts).
it was necessary
was shut down.
the same transmitter
at Millstone
sweep
i28 ‘t ionospheric
(Lowell,
This was accomplished
June 1973, when it finally
employing
employed
of a new HF ionospheric
cable.
Tbe
is sent
the
with matching
of the cables.
there
are no moving
construction
(except
parts
in the
for the transmitter
TmmzL
—
TAPE
RECORDER
-
oIGIcoDER
-
?:!;:?:
-
SYNTHESIZER
_
vENTILATOR
TRANSLATOR.
Fig. 1.
Photograph of the Digisonde
128 system showing the main components.
3
-..
---
,.——
.—
Fig.2.
Photograph of the transmitter power amplifier constructed
for the Digisonde 128 system using surplus C-4 Componenf$.
FREQUENCY(MHZ)
Fig.3.
EXampI~
of a record printed
I
4
4
by the Digisonde
128 sounder.
power
amplifier),
this insures
ment is that it provides
Figure
3 provides
hard-copy
an example
A block diagram
oscillators.
stable quartz
oscillator.
by internal
digital
interval
records
Thus,
of a frequency
soundings
frequency
steps.
The vertical
a train of 2N x 80 pulses
At Millstone,
The phase of the pulses
O“ or 180°,
receive
according
r local
The control
is made twice
dark lines
(N = i,2,3
,4,5...
per hour,
in each subgroup
of 80 pulses
is changed likewise,
receiver
signals
mediate
frequency
are converted
of 400 kHz,
The correctly
signal.
3-,
second,
sample
or third,
4.5- or 6-km radar
The median
this,
the samples
same<
values
so that the instrument
amplitude
allows
phase -coherent
,.,
Two adjacent
code,
amplitude
of three
gai”
range
year,
setting,
vided to introduce
mation
block.
date,
information
All information
amplitude
samples
IF,
or
on 1.5-.
on the lower
Thus,
memory.
decreased
or left the
of the digitally
measured
of signal-to-interference
minutes,
into characters,
is provided
is expressed
three
seconds,
on range
in Z56 increments.
sample
These
(phase in 8 increments
after
receiver
(Fig. 5).
which are part of the previously
in binary
form
one integra-
by ablockof
transmitted,
and density
and when combined
contain-
and the following
produce,
are preceded
frequency
delay
of six hits
by one phase character
octal bits (8 portions)
These
samPles
and amplitude
as one character’
the IZ8 height ranges
a set of i92. characters.
hour,
in a digital
to do
root of the number of samples,
are separated
5
—.-.—
of the iOO-kHz
to sampling
stored
convergence
to the square
the amplitude
octal bits.
andinfomnation
already
are measured
into a complex
phase measurement
(one frequency),
tion containing:
of the !OO-kHz
20 dB.
)
tio~ period
to an inter-
for each height range;
The improvement
is proportional
Using binary
ing the preceding
cycle
must be increased,
fast and optimal
of the amplitude
integration
values
amplitudes.
process
phase measurement
every
This corresponds
The
TWO samPles
of one cycle
and phase is determined
the value stored
or approximately
(or 64 levels).
in .28 height ranges.
so that either
with the reapecti”e
whether
ratio by this integration
in 64 increments),
phase coherent,
height increments.
weight function
after
IF is sampled
logarithmic
sin and cos components
are provided
which for N . ‘t is ~,
are con”erted
remains
amplifier.
periods
The sin and cos samples
I
The phase of the
receiver
are compared
decoding
pulse to pulse by
by
100-kHz
is selected.
on each frequency.
signs 1 is being changed continuously.
or fourth one can be sampled.
determines
A changing
after
the next frequency
SUI. rheterodyne
value of signal
This comparison
At each frequency,
by a shift register.
they are amplified
providing
reso-
of 0.5 MHz.
capability.
in a multiple-conversion
phase-decoded
Selectable
every
with 50-kHz
where
are taken in each beight range,
which
and was made using 50-kHz
is made to change from
but at the output, the phase of an unwa.nted interfering
frequencY
sounding fyOm
on the haIf hour,
are transmitted
code generated
can be
sOundings.
A cOmPlete
before
3Z0 pulses
i.e.,
are selected
The smallest
for E-regiOn
is its integration
are nO
an internal
of the synthesizer
the range 2 to i O MHz.
) is transmitted
is employed;
there
from
frequencies
denote frequent y intervals
to a pseudorandom
oscillator
and receiver
i to 4 MHz once per hour.
of the new ionosonde
N = 2 usually
Unlike the C-4,
(and time ) are generated
transmitter
shown in Fig. 3 covers
The most novel feature
in Fig. 4.
This option is emplOyed
range
2 to i6 MHz (or Z to !10 MHz) usually
The ionogram
is given
frequencies
synthesizer.
is 25 kHz.
of the new instru-
which foF2 can be read off easily.
but this has not been done at Millstone.
may be made over the frequency
lution.
from
feature
records.
system
the desired
computer,
A second desirable
in real time,
of one of these
All the required
control
to a local
between
reliability.
of the Digisonde
flee -running
transferred
greater
informagain,
MeanS are PrQmentioned
infor-
with i92 characters
\ -wI-16045
1
RECEIVE
RHmBIC
I
TRANSMll
RHIXWC
QY
PuSH-PULL
l+H
R’%%
W-MHZ
cRY2T,u
02CIIJA11X
.
RG9WLI C(IAX
c0MP851AT0R
+ D2TECTDR
I
t
1 II
I
MEWRY
2EOUEN-CER
SYNTHESIZER
I
1
r-
TRANSLATOR
OIGICODER
I
E&I
E&I
\
LINE
DRIVER
WSW=HWYERP
450G FT
OIGISONW
MDDIFIEO C-4
12s s/N1
Fig.4.
Simplified
block diagram
of the Digisonde
128 sounder.
TRANSMMES
1s, DATA SAMPLE
of data,
Fig.5.
Key to the intensity
preface
information
will form
memory,
I.evel code (top) employed
(center);..
one-tentli
generated
128th
sample record
of one record.
in the preceding
tioned above are transferred
through
reduce
At Millstone,
frequency
magnetic
output is employed
stepping
not be read out at 500 characters
speed.
This is accomplished
The preface
I
I
information
The printed
records
Lowell
Technological
special
type font,
value.
Thus,
picture,
large
any digital
device
identification
marker.
frequent y, while
ference
to achieve
records
tends to be lost.
below an adjustable
thus far,
elements
changing frequency.
results
technique
consist
blackness
shown in Fig. 5.
developed
of numerals,
is proportional
than,
from
can-
to slow down the sweep
(Fig. 3 ) in the manner
using a numeric
and the
the memory
say,
coding
using a
3 or 4 (Fig. 5).
standard
at
to the numeric
The
BCD data from
lines mark each tenth sounding frequency.
automatically
at the low-altitude
axis represents
the intensity
(z-axis)
range)
time delay
represents
give the log of the median
intensity
in part,
The station
end of each frequency
(viriual
height),
horizontal
echo amplitude.
at each height and frequency
some of the ‘Zcontrast ‘t between
This can be recovered,
threshold.
gaps
for the telecopier.
vertical
enough dynamic
men-
compatible
and record
(4 X 80) before
much darker
telecopier,
vertical
data have been printed
Since the printer
record
plotted
like 7 or 8 appear
suitable
320 pulses
that the apparent
Magnafax
black,
Preface
speed of the printer,
The picture
Foundation.
The axes are standard:
axis represents
(in order
on the printed
ionograms
into a form
In Fig. 3, the heavy,
over
provide
numbers
each ?requency.
have not been made routinely
appears
made on a standard
of the
information
per second,
per second and hence it is necessary
having the property
the contents
onto tape.
Owing to the slower
by integrating
Institute
time;
plus the peripheral
memory
Fig .3);
of the .p.reface.
rate to two per second.
tape recordings
instead.
showing location
at a rate of 500 characters
imk?gration time of O.4 second for
the maximum
printer
process,
a storage
The data are read cmt of.the memory
with the fastest
i. the icmosonde records (cf.
strip (bottom)
During the integration
eampling
DATA SAMPLE
by printing
echoes
and inter-
as ‘Izero It all numbers
Provision
to operate
the capability
35-mm
film
a storage
grams
copies
readily.
of the ionograms
tube display
produced
to the World
the C-4 sounder was maintained
of finding foF2 by sweeping
and camera
by the Digisonde
Data Center.
) At this point,
B.
Observing
puIse -pair
modes
employed
vided data.
system,
(The paper
operation
as this allowed
sent routinely
In addition,
to, the World
a means was developed
an observer
the C-4 provided
Data Center.
of photographing
the iono-
Fig. 3), so that we could continue to send film
records
Using
records
tend to be bulky and cannot be reproduced
of the C-4 was discontinued.
Procedures
During 1972, we attempted
newer
that were
(e. g.,
initially
the frequent y manually.
scheme
to make observations
at least
for the single
In normal
utes with 8 minutes
long-pulse
or ‘Iregular”
measurements
operations,
of data being collected
NORMAL
long-pulse
Table
11lists
and the altitudes
the cycle
A,
method and the
tbe Operating
over which these pro-
B, C was repeated
every
30 min-
in each mode.
TABLE
THE
using the single
once per month for 24 hours.
“ONE-PULSE”
II
EXPERIMENT
MODE
SEQUENCE
i
Pulse
Len@h
.,
uti.an
Sample
Altitude
Spacing
Coverage
Measured
(km)
(km)
(km)
A
100
15
7.5
100-1000
Power
Ne
8
500
75
30
150-1500
Power
Ne
75
225-
Power spectrum
Te,
30
300-2000
75
c
1000
D*
150
10+30
50
Direct
Deduced
Ti,
V
Power
N
450-1125
Power spectrum
T=, Ti,
V
30
150-
Power
75
150-350
675
503
Power spectrum
‘!
*Employed
with he
As described
L-bred
steerable
in Ref. 9, provision
radar during 2-D
z
‘d
to switch
rapidly
between
transmitters
tbe proper condition for the interface
equipment that transfers
data
24
to the computer.
During 4972, advantage was taken of this capability to switch
between
(in a program
radar
program
which
automatically
the radar
two radars
with a new data-taking
tbe L-band
established
rapidly
the computer
e
experiments.
was made in i97i
and reload
z
and UHF radar
from
1
Parameters
(psec)
Mode
‘1
Height
Red
operation
of the L-band
of propagation
studies)
cannot be employed
interface
equipment,
radar
employed
and incoherent
simultaneously
and the computer
to track
scatter
the Navy Navigation
operation
as the transmitter
of the UHF radar.
cooling
all are shared. ) These
Satellites
and power
mixed
(The
supply,
operations
the
{termed
I
I
i
STATS
for Satellite
Tracking
and Thomson
Scatter 1 permitted
once per hour and hence afforded
less time
resolution
the longer
completed
successfully
STATS
A second
to resolve
variations
field
to measure
measures
all three
the vertical
radar to measure
111).
Table
from
meridian
In this direction,
112
-Dt! and were
(termed
in the magnetic
the beam is almost
all the observing
that attempted
parallel
of pressure
Sine
meridian
the UHF radar
to secure
meridian
to the field
lines
the L-band
a second inde -
could be recovered.
For most
at {5°
elevation
at F-region
in the magnetic
for which useful data were
for later
only to employ
in the magnetic
normal
a precursor
“ 3- D“ ).
111)the beam was directed
periods
here.
plane into components
it was necessary
antenna wa8 directed
(Table
from
by the E-W cOmpOnent of the F-region
here
of the drift
of the drift
Only the results
under the influence
which the two wanted components
the L-band
on two occasions
III lists
(caused
( Vz ) of the drift,
one component
2-D measurements,
However,
field
are termed
components
component
pendent measurement
(Table
to tbe magnetic
B, C to be completed
was in observations
by neutral winds and diffusion
These measurements
A,
runs.
are included
capability
of the ions in the magnetic
(caused
) and normaf
field).
attempts
of this rapid switching
the drift motions
to the magnetic
electric
runs that were
application
a cycle
than regular
gathered
heights.
E-W direction.
and are presented
in this report.
The 2-D sequence
D-mode
C.
(4 minutes),
B-mode
previously,
20
no attempt
as this would be too time consuming.
as functions
of range and frequency
along with other pertinent
of the run,
A profile
is the range)
While
alert
ceiver
usually
phase locked
data for the vertical
could detect
velocity
was not operating
the “ertical
velocity
Values
half-hour
Examples
on some
TOg ether with a PrintOut ‘f
spectrum,
this allows
of the equipment
frequency
synthesizers
frequency
days appear
the data
standard
from
the printout,
employed
in the re-
would not he evident.
each synthesizer
so scattered
This appears
properly.
For this,
in routine
reveals
in turn.
Despite
as to lead one to suspect
to be the case for i2-i3
a plot of the F-region
the values
obtained
operation
any errors
that is necessary
closest
in scaling
and entered
July and
from
the smooth
9
curves
critical
from
the Millstone
Including
ionograms,
valw?s from
frequency
and Wallops
to Millstone.
the local
if any half-hourly
into the computer
are scaled
at Ottawa (45-N)
of these plots have been included
for fnF2 are scaled
intervals
Printer.
to monitor
in the plots are values
usually
to guide the interpolation
for any reason.
as it
collected
start time, and duration
-2
dependence where R
for the R
corrected
the data is to construct
which are the two stations
stations
(i. e.,
of echo power
data for these days have been discarded.
step in analyzing
Also included
these
and
tape at the end of each integration
malfunctions
was provided
foF2 vs time for the days of observation.
(38 - N),
(i. e.,
out by a high-speed
to the site master
counter
drift
the data in real time
the samples
on magnetic
of any (of three)
a frequency
The first
Instead,
at each point within each frequency
that the receiver
from
(8 minutes),
while they are being gathered.
operators
to remnin
iormgrams.
C-mode
40 minutes.
such as the mode type,
vs height
and printed
such as the failure
Accordingly,
this,
ratio
to be monitored
subtle effects
are stored
information
of echo power
is computed
the signal-to-noise
quality
every
is made to analyze
is gathered)
period
(4 minutes),
approximately
Reduction
Data
As described
I
was A-mode
( i6 minutes ); this could be repeated
Island
values
and can serve
Millstone
in a number of pre”ious
are missing
4,5
reports.
drawn through the points on the plots at
via punched cards.
These
are stored
and used
TABLE !11
INCOHERENT
End
Begi.
c*
Date
25 January
EST
DcJte
1220
26 J.nuary
-
c“
EST
Mean
Kp
Ob,t
D
1240
4-
Reg
I 500
3
2-D
1972
Cwnment
Az-252”,
EI =15”
Az =345”,
El=15°
26 January
D
I 350
27 January
23 February
Q
0950
24 February
D
1150
3+
Reg
? March
I 000
10 March
QQ
low
I
Reg
23 March
I 620
24 March
D
I51O
3+
2-D
1600
27 April
1700
1+
kg
I 230
10 May
1330
2+
Reg
1130
26 May
1300
2-
STATS
Gap 1600-2D30
0920
31 May
10IO
3+
2-D
Az =345”,
El=15°
1710
1+
STATS
QQ
26 Apri I
,
SCATTER OBSERVATIONS
9 May
Q
25 May
30 May
o
o
B J.ne
Q
1020
9 June
13 June
Q
G920
14 June
1100
2-
Reg
1030
29 June
0500
2+
2-D
Az =3450,
EI =150
1150
I July
Q
I 200
I
2-D
Az =345”,
EI =15”
0850
13 July
QQ
1020
I
Reg
Nonvertical
drift data
1020
27 J“iy
1420
2+
2-D
Az =255”,
EI =30”
1110
2-
Reg
Az=345°,
EI =180
2B June
QQ
30 June
12 July
D
26 July
QQ
o
o
7 August
0920
B August
6 Septembsr
1010
7 September
1300
2-
2-D
Q
0820
13 September
Iloo
2-
Reg
QQ
0810
Q
Iolo
1+
F&g
D
0930
16 November
D
1630
4
2-D
QQ
0930
7 December
1600
2
12 September
3 October
15 Ncwemter
6 December
4 October
Q
0
2-D
Gop51530-1900,
0300-0500
A2=345”,
EI=15”
, Condition:
QQ
Q
D
Oneoffive
quietest days i.ma.th
Oneoften
quietesfd.ys
inmanth
One of five m.xtdlsturbeddap
in month.
tObservOtiOns:
Reg=Reg”lar.
2-O=
.nd Thomson $ tatter.
L-band and UHF r.adormeas.rernentsr
STATS =Satellife
Trocking
to obtain the value of foF2 at the midpoint
program
combines
measurements
each cycle
of observation
of electron
density
variations
in the ratio
electron
Te/Ti
for electron
estimates
profile~t
and normalizing
interpolation.*
B-,
This is converted
for the effects
The
and C-mode
runs in
to an absolute
profile
on the backscatter
the reaulta.nt curve
and ion temperatures
0+ is the only ion present.
when sufficient
‘!power
by allowing
run by linear
made with the all A-,
power
of altitude
to have the correct
value of
(Nmax )t at the peak of the layer.
density
Values
into a single
vs altitude
of each A-mode
of echo power
This assumption
H+ ions may be present
unreliable.
More
(private
communication,
altitude
(Sec. IV).
are recovered
accurate
is a good one except
at altitudes
values
below
to recover
this program
the spectra
consumes
that
the temperature
using a program
Te,
assuming
at night near sunspot minimum
900 km to render
can be obtained
*976 ) which attempts
Unfortunately
from
Ti,
due to J. L. Massa
and the H+/Ne ratio
a considerable
at each
amount of computer
time and hence is not run routinely.
It has been foundzo that estimates
differ
at night in summer
It is believed
that the discrepancy
spectra
of the signals
introduced
spectra
are narrow.
In principle,
employed
are less perfectly
correct,
modes
matched
B-mode
more
center
from
scheme
was employed
ture were
corrected
correction
relator
(INSCAL)
allowing
of variations
bias errors
here.
of the changing
susceptible
which attempts
represents
the time
results
. . . .... .. -—..,—..-.v..mi-
el/cm3
the results
Finally,
to correct
the
performed
a
in the effective
Emery
found that the cor-
depend not only on the
correction
reported
the values
analyzer
as a source
to recover
scheme
was
for 197’t.9 The same
for electron
Ne,
was replaced
of systematic
Te,
of height variations
in a truly
only a first-order
chosen . start time
t Nmax = 1.24 X i04 (foF2)2
the data in the two
but to a Ies ser extent also
continuous
with the ANALYSIS
at some times,
data.9
in the B-mode
is
tempera-
Debye length with altitude.8
bank spectrum
on the Ne profile
in the B-mode
the C-mode
B. A. Emery
in the C-mode)
A smooth
in Ne (via the Debye length correction),
in ANALYSIS20
it is believed
(to allow for differences
obtained
Since
in the B-mode
Assuming
Subsequently,
to correct
reported
cannot be analyzed
has been written
for the influence
employed
* Actually,
to be less
with this device
at such times.
analyzer
by comparing
using two years’
value).
in 1976, the analog filter
that is believed
gathered
spectrum
scheme
heights
values
and employed
for the results
for the effect
at night when the
for this by the method
must suffer
estimates.
for Ti.
of the frequency
particularly
pulse than those in the C-mode,
(taken to be that observed
this comparison
Beginning
.-
in the receiver
several
to be the C-mode
derived
(B-mode)
accuracy
in 1969 and 1970?’8
employing
value of Te/Ti
amount of smearing
pulses
data tend to
in the estimates
height on four days,7 and this was employed
to tbe Ti and Te/Ti
on Ti (again assumed
the large
in the B-mode
an empirical
gathered
from the B- and C-mode
are made to compensate
employed
are primarily
comparison
to be applied
prevailing
_
attempts
height of the pulse for the two modes)
rections
,,
from
but the measurement
at 525-km nominal
temperatures
detailed
obtained
This leads to differences
to the transmitter
errors
J. E. Salah derived
gathered
stems
that the filters
that the systematic
- i. O.
using O.5-msec
20
in the data analysis,
it also was evident
of Te/Ti
when Te/Ti
program
error.
of Te/Ti
The data
of height,
and on the Te profile
self-consistent
elaborate
fashion.
: C—-,F?,
That
but in view of the possible
approach
seems
unwarranted.
+ 4 minutes.
when foF2 is expressed
cor -
and a new program
and Ti as functions
correction,
a more
by a digitaI
in megahertz.
asE3am?&ws”w:.5
.
MI LL3’[ONE
HILL
25-26,
JFIN, 1972
L13G,0N[
(d Log, ~ Ne
Fig .&a-d).
.
Results for 25-26
January
1972.
The next part of the analysis
peratures,
and vertical
performed
by fitting,
velocity
estimates
the data.
in Ref. 8,
simply
height),
effect
but is shifted
not inci”ded
(including
routinely
A subroutine
here)
of the INSCON
section.
In addition,
variation
of any parameter
covered.
INSCON
program
pro”ides
These,.
together
be. obtained
form
sented
but was
tape to drive
a Calcom.p plotter
are given in the next
uf the. polynomial
fit from which the
(within the period
with a listing
program
fitted)
can be re -
tape which is trans-
given here as Appendix
(R C.VR)
allow
numerical
A.
Val,les
tO
by other Users.*
DENSITY;”
contour plots of Ne,
in the manner
for the days listed
of loglo
Ne (el/cm3)
abo”e
aPPears
ELECTRON
outlined
ANDION
TEMPERATURES,
in Table
hn,ax F2 sometimes
to be increasing
are encountered
(shown as broken line) where
taintyin
determining
night when tbe echoes
It is believed
scheme
allows
for example,
2 hou-s,
(typically
the normal
internals,
very
diurnal
10gio Ne ~3.o.
owing to experimental
is greatest
uncertainty
At higher
contributes
of Ne are labeled
have been edited from
these plots
time resolution
variations
Ionospheric
smoothed
for electron
respectively.
rapidly
Contours
error,
the density
the plots,
but in
in the vicinity
of
is set chiefly
altitudes,
to the overall
in units
RegiOns
however,
uncertainty
by the uncerthe uncertainty
–especially
at
are weakest.
that the 30-minute
are effectively
where,
“1’hese usually
*0.2 MHz).
of. aRitude and time. have
in Ref. 8); these are pre-
Ne = o.2 wherever
the experimental
measurements
by Traveling
‘rbe results
increases
foF2
scatter
in detail
through 26.
The acc.racyof
real.
h~axF2
in the incoherent
(and described
fll in Figs.6
with altitude.
~ .a:f unctions
‘YtiTi,and’v’
above
and are drawn in steps of logio
any case are not considered
by the measurements
provided
to be followed
Disturbances
(TIDs)
by the ‘rregular!’
adequately,
measurement
but fluctuations
witb periods
of lesithm
caused,
about
out.
and ion temperatures
The
at sunrise.
sented in the plots gathered
afforded
This
profiles,
for i970 and subsequently
‘f?i, and Vz. These
the coefficients
FQRT:RAN”recorery
‘!nom inal])
General
Computer-drawn
100-K
published
a plotting
Te,
(in f30ulder) together
in machine-readable
been generated
well
density
for each day are combined. on a single
Data: Center
with a simple
height for tbe pulse is
with delay within the pulse.
as a function of height or time
111.”’RESULTS
FOR ELECTRO.N
AND” VERTICALVELOCITY
A..
of Ne,
and has
in the profiles
the so-called
tbe electron
is
surface
for this effect.
produces
diagrams
The. sets of coefficients
to tbe World
for distortion
(i. e.,
The results
have been corrected
which is used to. obtain contour
mitted
of echo power
for tbe plots of Te and Ti.
those presented
This operation
polynomial
center
are sampled
is taken into account in constructing
and ion tern -
this is known as lNSCON,
can compensate
by tbe fact that the effective
owing to the variation
electron
a two-dimensional
that performs
program
density,
of height and time.
sense,
by the time at which the echoes
automatically
the electron
as functions
Tke program
The INSCON
of Te and Ti vs altitude introduced
not given
smoothing
in a least-mean-squares
that best represents
been described
involves
electron
temperature
It is possible
for the STATS
was reduced
are presented
exhibits
a large
that this rapid increase
observations
to -i
as isotherms
(Table
at 200 °K and
diurnal
variation
is not properly
111)where the time
and
repre-
resolution
hour.
,
,.i
I
.—
LLSI
;-26.
ONE HILL
JRN, 72
,m
?m
(b) T=,
Fig.6(a-d).
Continued.
MILLSTONE
HILI
25-26,
JRN,72
.
,m
,1
,m
,m
xc
:Gc
–-~---”-i—–-’–r—n
,“
__T;..-..—____
___
J
--”n;–””—~—~:—--[~n~n---
(c) Ti .
Fig. &o-d)
Ccmti. ued.
\,
_T———
,,
MILLSTONE
HILL
25-26,
JRN. 72
!,
,00
“z
__: ___...-.._.-.—._—r
_____~–
...._–—[.
.—.._l.:._
Fig.6(a-d).
. .. .
..r.–—–._~
L
,.
\,
.
Continued.
,..
.
MILLSTONE
HILL
26-27,
JFIN, 1972
LOCIONE
~
m.
m
,m
“m
,,,
,,
.
..... .......
.
. . . . . . . ...”””””””
>
.
..... ...
,.L=[it(ii&xi
?,..,
..........
>p~~
m
5
7
-!?5
,
EST
(.)
I
Fig.7( a-d).
h
‘
%,0
N,.
Results for 26-27
January
1972,
L
L
L
\*
LLSTONE
-27, JW,
WC
,m
x.
:E.c
HILL
1972
LLSTONE HILL
-27, JRN. 1972
s
L
,7
rT~–TT-
1,,
(c) Ti .
Fig .7(a-d).
Continued.
~“-~,—-—
\,
3
1
!,
ILLST13NE
HILL
;-27,
JRN, 1972
-@mm
(d) V=.
Fig.7( .-d)
Continued.
I
I
!
I
MILLSTONE
HILL
23-24> FEB. )972
L13C,ON~
=
.-
“r””
__
I
u]“’:’
\.;:..
‘~l
‘“2>EJ
““”””’”””’””””””””””””””’”’’”’”
““’””
z“
+0 1..b?
>
T—”–--”-r
x-—
– ,7
~’+
(d
Fig .8(a-d).
.
&
Log,.
N,.
Results for 23-24
February
1972.
s
“k”
‘u.
‘“
~
FlILLST13h4E HILL
~3-2q,
FEB. i972
_EEl-
.
.
.
w
.
.
m
.
w
m
xc
.
%3
m
%
m
K@
(b) T=.
Fig .8(a-d).
——
. . . . . ..
.
..
,.
Ccmtin.ed
.
-
MILLSTONE
HILL
~3-24,
FEB. i 972
~
,m
..-
‘i
I
(c) T;.
Fig.8( a-d).
Continued.
:LLSTONE HILL
)-24. FEE, i972
..- .. ...- V-...–-–.K
–T.–-–.
i,
!1
b.?.x4-
l,, ~t~
J-=
L::
(d)Vz.
Fig .8(a-d).
Continued.
L
b
L
L
L
13
LW.., CN,
<J’”’
w
.,.
N
.
T..
,,
!,
(.)
Fig .9(a-d).
Log,.
N, .
Results for 9-10
March
1972.
LLST5NE
HILL
-10. M!WI972
[-00-160801
‘/-’/”~
\lllll\
///-
(b) T,.
Fig .9(o-d).
L.
.. . . . .
.. .
:.,-
Continued.
.-——
-EmmiL
LLSTONE HILL
-10, MRR. 1972
N
.
(c) Ti .
Fig .9(a-d).
Continued.
I -“””
LLSTONE HILL
-10, YRR. 1972
~
‘,,
[
/
,
()
N
.
\,
L
L
7
L
~J
L
(d) V=.
Fig .9(cj-d).
...,- .... ..
Ccmtinued.
L
k
MILLSTONE
HILL
23-2Li.
MRR, 1972
LOG>n N[
,m
L
,5. ,
.—.
.._
“’’’’/’’/...
I .>’’’’’’’:-,’’”’’’”’’’{”’”””
-----
‘,2
(.)
Fig . Iqa-d).
Log,.
Ne .
Results for 23-24
March
1972.
‘---’..
.—
\“
I -ml&064]
MI LLSTUNE
HILL
23-2Ll.
MPR. 1972
WC
1[
—
/
!8
c
2
L
#
L
EST
(b) Te.
Fig.lO( a-d).
Continued.
k
,
~)
o
L
L
r
ILLSTUNE
HILL
3-2LI , ?lWI, 1972
-LST13NE HILL
-24. MFIR. 1972
.
K
(d) V=,
Fig. Isa-d).
b
.
.
.........
Continued.
m
. .. ... . .. ..
.. .,4
.7..
.. .....
. .. . .. .. . . . . ... .
4
!IILLWON:
2627,
Wfi.
[ -00-16061
HILL
1972
(.) Loqo
Fig.ll(a-d).
Ne
Rewltsfor26-Z
April
1972.
I
1-00 -16068[
MILLSTONE
HILL
~6-27.
9PR. 1972
.
i
L
L
1
ESi’J’O°
\
!
\
\
\
‘“”
(b) Te .
Fig, ll(wd).
.,..,.... .. . ...
Continued.
m
-------4
MILLSTONE
HILL
@27,
9PR, 1972
1–00-16069
(c) Ti
Fig.ll(a-d).
Continued.
[
# p
MILLSTONE
26-27 >WR.
] -00-16010
HILL
1972
:L-,o
,2
,
,,
,
,
k
0
L
L
L
I
~~
E;
(d) V=.
Fig.1 l(cj-d).
-,, .= .. . . . .. ,..=..
Continued.
.
.
. ..
,..
.... ... .......
..... ...... .. .. . . . . .
‘U-
4
k,
m
<.(G>”’’D)>
/--’
x!
:6
(d
Fig .12(a-d).
b,oNe.
Results for 9-10
May
1972.
/-’’-’-’”
[ –DO-1601?1
LLSTONE HILL
-10. MQY,I972
.
70?
WC
,W
.
.
!.
‘b
-.
... . ...
MILLSTONE
HILL
9-10. MRY. 1972
T.
1-00-16073]
xc
cm
xc
m
,fo
Fig
12(a-d).
Ccmtinwed.
L-00-16074
LLSTLINE HILL
-10. MRY, 1972
.
m
T:,
3,.
.
:m
Fig.12(a-d).
Continued.
I
4
? I –00-1801s
MILL5TONE
H [U
25-X.
!IRY, 1972
,.,
>5.0
.
3.6
.,,
,. .,,,.,
.
.
. .
.
EST
(0) Log,. Ne.
Fig. 13(.-d).
Results for 25-26
May
1972.
1
\ -00-1601$I
.LSTONE HILL
26. MRY. 1972
em
xc
x
x
–T:__._[=.._..r
:!
L
s
I,,
L
L ~
L
(b) Te
Fig. 13(a-d).
Continued.
. ..
..r..r_7._
p=-=’-
““’’’:-’
..
MILLSTONE
HILL
~5-26,
W7Y, 1972
] -90-16077]
~ ,.L.
/
//5//
\
L
,
L
,
..
L
4
k!
F“S;
(c) Ti.
Fig. 13(a-d).
Continued.
L
k
b
,
\,
,
I -00-16018
MILLS1ONE
HILL
25-26 .!19Y. 1972
]
v.
,m
/
I
T
-——-----.
“.-
..=...,.
-..
Am
[-00-16019
MILLSTONE
HILL
30-31 ,!I!4Y. 1972
LOC,GNC
m.
,,,,
.“. ”
,s.,
‘4.,
\.
\,.,
,..,
.!.,
,G
G-”
L,.”
m
“.-..,
,m
.,.
-
(o)
Fig. 14(a-d).
Log,.
Ne.
Results for 30-31
May
1972.
,,
M“---’””
“,”
I
MILLSTONE
HILL
30-3i.
!lRY. 1972
m
1 -00-160801
‘“’
NNE
/
L,,,.,
II,
\,
1
.,
f:,
L
k
~~~.
(b) T,.
Fig. 14(a-d).
Continued.
1:
L
k
L
k
i,
MILLSTONE
HILL
~0-3i,
?lRY, i972
1-00-160811
.
\Y\\\\\\
ma
,m
m
(c) T..
Fig.14( a-d).
Continued.
MI LLSICNE
HILL
30-31 >!IRY, 1972
1
Fig.lqa-d).
Continued.
1
1.
L
L.
(,
I - 00-16083[
Pl[L LSTONE H [ LL
O&09 , JUN .1972
LOf&Mc
m
.
,,
.
,(,
.... . . ..
,,.”:+>~~
.-
.,.,,, .. . . ....”
,.. ..’
.,.
.
0
,.
/
(,,
I
1.
!.
/
/
k
L
L
EST
k
L
(.)
Fig. 15(a-d).
f
\
.
k
k
L0910 Ne
Results for 8-9 June 1972.
b
10
\..
!2
/
,---”-
.“”’ I
/ \
S-2
I
LLSTONE HILL
-09, JUN. 1972
.
.
:.
(b) T=.
Fig. 15(a-d).
Continued.
l-no-mast
MILLSTONE HILL
08-09. JUN. 1972
.
.
,8
(c)Ti.
Fig. 15(a-d).
Continued
MILLS1ONF HILL
08-09, JUN. 1972
,,.
] -00-160861
,,
I
.
1
.
“a-l
L.
(,,
,.
(.
,0
,.
1.
,“
L.
1.
~~yw:?b<k
I
b\o\,
\“
b
(d) V=.
I
Fig. 15(a-d).
..:..... . . . . ..
Ccmtinued.
(
1-00-160871
!lILLSTi3NE
HILL
13-14 .JUN,1972
I
I
5.,
—
~’””
~b ......>
...\.....
~/*;=~G:
-
.0
k
,,,
b
,),
,,
s.”
J.
,,
21—
73
.
EST
(o) Lw,
Fig .l<a-d).
o Ne
Results for 13-14
June 1972.
m
05
m
m
)>
I
~~
ILLSTONE
HILL
3-1~, JUN,1972
L-Do-160881
.
.
,m
,.m
.
-~ -..-,..--.~.- .-----~
MILLSTONE
HILL
13-114, JUN,1972
T.
] -00-160891
.
.
,,
,.
,,
,,
,,
‘b”
dn”mb
(c) Ti .
Fig. la.-d).
Continued.
IF
1
ILLSTONE
HILL
3-l U. JUN. 1972
.
\!
L
L
7
k
L
k
k
d
(d) V=.
Fig. Itia-d).
Continued.
..-.s
““~’
‘“
““”””
..”.
L
L
.,
L3
-DO-16090\
L
. ..-.:, :,—.—. .——.
-. . .... . . ........ ... .-.. ..:,... -—..4
—...-.
....__ . ..._.
~
.
.~-.
~ -
...
.. .
MILLSTONE
H[LL
28-29.
JUN. 1972
I flc.. N.Uu
,“
f’””
1(“bsln
‘..
y
1’ Y
c“”””
fi,,o
am
.;
/
.s.o—
.
..5.,
,m
—
‘!0
I
>,
.
1–00-18091
,.,,
\
.-
1
).
1
,6
1
),
1
1
z
~$ymmmm
(d
Fig.17(a-d).
Log,.
I
1
m).
N,.
Results for 28-29
1
June 1972.
.. ~..~~-.
I
.LSTIINE
HILL
-29> JUN. 1972
[-00-18092
I
-. —.
—.... ., ....
.:....~,:.::
-... .—.,...A.
.X&:-..
. .
..-.L. —-.
,:—..
—.. .—.—::
A-..
-—--L.QA:
.-..,..
.. . .... .
.< ..
... .. . .. . . . ,-. .
.
i..
1-00 -16093[
LLSTONE HILL
-29, JUN. 1972
(c) Ti .
Fig. 17(a-d).
Continued.
I
MILLSTONE
HILL
28-29
JUN. 1972
,,
!,
i“
\,
!*
$0
&
~
(d)Vz.
Fig. 17(a-d).
Continued.
*
b+
w
t-u
-00-160941
,0
—.. ..—.—
m-
.. .......... ... ,...—
-..--:
.
. .,
,.
MILLSTONE
HILL
30JLIN-OIJUL
, 1972
LEC,ONK
1-00-16095
m
Gm
,m.
.
160
(d
Fi9. 18(a-d).
Log,0
N,.
Rewlts for 30 June -
July
1972.
I
[-Do-18098
LLSTL7NE HILL
JUN-OIJUL,
1972
Fig. 18(a-d).
Continued.
[
LLS1”ONF HILL
lj!JN-Oi Jli. , 1972
L’
.
,s
!5
,0
5
‘.3
3,.
,
L
I
t,
A
4,
~5+
~
~:
k
.,
(d) V=.
Fig. 18(a-d).
Continued.
—.
,
L
,
..
,=.. . .. . ..
.——
.
.,&
MI LLSTUNE HILL
12-13,
JUL,1972
LOG,.Nr
m
m
.
z
,..
,.
EST
(4
Fig.19(a-.).
Lwlo
Ne.
Results for 12-13
July
1972.
.
I- DO-161OO[
LLST13NE HILL
-13. JUL,1972
.
-“l
/“’//////1//
.
.
:,
I
(b) T,.
Fig. 19(a-c).
Continued.
MI LLSTCINE HILL
~2-13.
JUL.1972
am -
I -00-16102 I
II ILLSTONE H t LL
26-27.
JUL, 1972
LOG,ON~
EST
(o) L0910 Ne .
Fig .2C(a-d).
Results for 26-27
July
1972.
I -DD-I81031
MILLSTONE HILL
26-27.
JUL. 1972
cm
.
xc
.
:.
(b) T,.
Fig .Zqa-d).
Continued.
MILLSTCTNE HILL
~6-27,
JUL. 1972
1–00-16104[
m
w
(c) Ti .
Fig.2D(a-d).
Continued.
.LS113NE HILL
-27, JUL, 1972
[- BO-161O5i
.,.
.
:m
(d) V=.
Fig.2Ma-d).
Continwed.
-,8- 1s,0$
MILLSTONE
HILL
78. WIG, 1972
LOG, nN.
w.
70)
.
m
\/’
--- ““ /
,,
,,
IS
,,
,,
ES~=n’n’n’
(a) Log lo Ne.
Fig .21(cr-d)
.
Result, for 7-8 August 1972.
‘m”
I
6s
,m
hli LL!51UNE
HILL
.78> RUG 1972
c’
—“—
“-.-/-’-
(c) Ti.
Fig.21(a-d).
Conti.ued.
MI LLSICJNE
HILL
78, WJG, 1972
Vz
1-,0 -1610,1
m.
xx
b,
\3
,,i
)7
k.
>,
,,,
F:!+
(d) V=.
Fig.21(a-d).
Continued.
b,
05
m
*,
1!
m.
I -DO-1S11OI
MILLSTONE
HILL
6- 7, SEP+ 1972
LCiC,ONE
.
4.,
.
m
Em
(d Log,.
Fig .22(a-d).
N, .
Results for 6-7 September
1972.
MILLS1ONE
HILL
.67, SEP, 1972
-4
4
I -00-161111
I -00-161121
HI LLST13NE HILL
6– ?. SEP. 1972
T.
Fig .Zxa-d).
,...
.. . .. .. .. .......
. .
Continued.
MILLSTONE
HILL
6- 7. SEP. 1972
v.,
1-00-18113(
,lcc
m
m
*m
\*
\,
i“
),
\,
5,
b
b
ES?
(d) V=.
Fig .22(a-d).
Continued.
b
k
b
io
i,
{ -DO-15114
i
!11LLSTL7NE HILL
12-13,
SZP, 1972
LLIC,ONC
m’
m
am
,672
*
(0) Log,.
Fig.23(a-d).
N=.
Results for 12-13
September
1972.
MILLSTONE
HILL
12-13,
SEP, 1972
1-00-16115[
,02
.
4
2
(b) Te .
Fig .23(a-d).
Continued.
I -00-16116
LLSTgNE
HILL
‘-13. SEP. 1972
-K
—
o
L
“
,
6
&
kc
~
(c) Ti .
Fig .23(a-d).
Continued.
L
..
L,
L
k
!,,
[
MILLSTONE
12-13 .SEP.
i,“,
1-00-161171
HILL
1972
m
\,
b
1,
h
\,
b
h
ES?
(d) V=.
Fig.23 (a-d).
Continued.
k
t.
b,
b
!0
,2
MILLSTONE
HILL
3- LI, CCT. 1’372
n.
.,
LW,OIYE
.
,.,
“.,
,.,
-’r---
,.,
-7--——
Fig .24(a-d).
i
I
1
.—.
Res.lts for 3-4
October
1972.
!IILLST”ONE HILL
..3q. 13CT. 1972
MI LLSH3NE HILL
3- IJ. CCT! 1.972
[-00-161201
‘“’’’m’”
‘“”””
?_-~\~;;;;
m
>,
,*
>s
,6
&2kw
L.
(c) Ti .
Fig .24(a-d).
Continued.
,
zm, ,,m ,2,02
,2103
,,q
Wm,o
,*x@
,Nm
<
MILLSTONE
HILL
3- 14. CICT, 1972
v.
j -00-1612!I
5?2
,m
.
m
X0
,s0
(d) V=.
Fig .24(ct-d).
Continued.
.
.
.
.
,,
(a) L0910 N=.
Fig .25(a-d).
Results for 15-16
November
1972.
,.
LLSTONE H [ LL
‘16, NW,1972
1-DO-1%123
I
.
\T l$flTT\T\-
vim
/
w
‘m
L7
,x
/--
“/’’/-’--”..
(b) Te .
Fig .25(a-d).
Continued.
] -00-16!
LLST13NE HILL
-16. NOV. ‘1972
.
.
=---.
%
\
‘“
“3--2X.
(c)Ti.
Fig .2S(a-d).
Continued.
241
LLSTONE HILL
-16) N13V,1972
I
WI
..*
/_-
(d) V=.
Fig.25( a-d).
Continued.
-00-181231
?lILLSTUNE HILL
6“n 7.., DEC.1972
.0
w
4’
h
1,
!s
$,
i,
~~;
k
(a)
Fig .2~a-d).
k
bbtrb
kll,
Log lo f’+e .
Results for 6-7
December
1972.
k
-LST13NE H ILL
- 7. DEC. 1972
-
,Y+m
/
L---”-m
.
.
El
*
m
.
(b) T,.
Fig .26(a-d).
Continued.
.LST13NEHILL
7. DEC.1972
=
/
\\\\\\~
,m
W
.
,.
,3
(c)Ti.
Fig .26(a-d).
Continued.
—,..,...
. ..—
—.—
.—.
..—
—..
.——.
-.—
..
..
.
-..
_..A
Y
.
“-EEL
LLSTONE HILL
- 7, DEC,1972
.
em
L
\,
,
1
.7
L
&
L
h
L
(d) V=.
Fig .26(a-d).
Continued.
L
L
!n
L
L
\,
The contours
of vertical
velocity V . are plotted at intervals
“chirp>’ introduceti by the transmitter.7
rectf?d for tine frequency
a. cle”at ion of 88° due south, the drift
component
cisely
the cfistirlctio.
“ertic al,
Values
but for most purposes
of the drift
quite unreliable,
data have,
observed
with
Accordingly,
however,
J..-band
polarization
electric
and
been cor-
have
beam is directed
that is measured
at
is not pre-
is unimportant.
rsdar
by Kirchhoff
ITI/SeC
Since-the
of the plasma
these measurements
been employed
tion of the ionospheric
26
the
of 5
usually
were
very
at night and
scattered
have not been included %“ this repor?.
and Carpenter
field over
These
ia .s study of the diurnal
Millstone
a..d its dependeme
var:a -
cm ms.gnetlc:
activity.
During
Despite
i’?i’2,
this,
disturbed
tbe 1?,.,7 solar
Quiet Winter
‘Pbe.e
quiet-time
Millstone
that has been discussed.
exhibitsa
pr-onounced diurnal
ni,ghtti.me densities
the L.-1ayer
thermosphere
by a factor
is formed
lower
reaches
a minimum
to explain
s“”lit
maximum.
ideas
demity
of all levels
in the results
As SW-
ITI addition,
of the
presented
here
Millstone
papers
during
a“d reviewed
many quiet winter
NrnaX declines
“r.ypically,
3,6,27
nights.
during the evening
The density then may remain
mmtmt
in
This
and
for many
reaching
the timing of the i“ci-ease
tlumugbout the winter
near midnight
theoretical
by noting that the conjugate
night and perhaps
when the solar
The subseqLleI1t cooling
Subsequent
ze”itb
of the field
the heat flux into the tuhc of force
distance
at the conjugate
tube then caused
and experimental
point to Millstone
work (reviewed
reached
point reached
the flux into the local
re-
its
iono-
in Ref. 7) have shown these
to be untemble.
We now believe
of the diurnal
that the timing
“ariation
of the event can be explained
of the exospheric
while that of neutral hydrogen
cause the charge
exchange
that the protowospheric
C.
Disturbed
At midlatitudes,
fOr example,
neutral
atmo,sphcre
reacticm
from
Winter
in the thermosphere
H+ to O to proceed
a“d large.
as a consequence
its mi”imurn
We
most rapidly,
discuss
this fllrtber
at about
is at a mitli -
This is just the condition
is at a maximum.
flux is dowmmrd
quite simply
This reaches
temperature.
0300 L,T with the result that the abundance of atomic oxygen
mmn,
(see,
also.
the
and 26(a).
in a number of previous
midnight.
in summer
less pronounced.
can be detected
24(z),
exceeding
a peak between 0200 a“d 0400 local time (LT).
Our earliest attempt
27
tbe phenomenon
was to invoke a downward flux of ionization from the magnetosphere.
its minimum
sphere.
density
becomes
as the neutral atmosphere
15(.J, .18(a),19(a),
after
near h~axF2
densities
the midday
variation
in Nmax that occurs over
We sought to explain
mains
in altitude
a little
behavior of tile ioiitisphere over
5-9
In winter, the electron density.
reports.
of $0 and exceeding
this seasonal
i. Figs. 7(a) and 26(a).
hours or increase
somewhat
3.).
with the daytime
feat. re,.. discussed
Ref. 7, is the increase
is evident
was appi-oached.
that were
winter and summer
Bath of these trends
is reduc. cl.
a study of Figs. 9(a),
feature
111exceeding
in many previous
variation
is approached,
One interesting
in Table
six days
Behavior
is a characteristic
spot minimum
as sumspot minim.m
to have been made on at least
(i. e.., with mean I<p give”
B.
from
flux Ccntinued to decline
observations-appear’
necessary
thereby
to
ensuring
in Sec. V-B.
Behavior
magnetic
storm
effects
tend to he less
Pr61s.28)
and this is thought to indicate
resulting
from
tbe storm-induced
pronounced
in winter
that the composition
changes
than summer
changes
i“ the
in the therm ospb. ric wind system
are more
arises
pronounced
because
sphere,
the auroral
because
larger
in the summer
heat deposited
the2~ailing
joule heating.
tron density
At all event~,
electron
large
at Millstone
tend to be the presence
hemisphere.
during the storm
ionospheric
are uncommon
turbed acti”ity
than the winter
is greater
densities
of large
hemi-
and this leads to a
depressions
and the most obvious
TIDs
that this
in the summer
are larger
stm-m-associated
i“ winter
We have suggested
of the daytime
manifestations
and/or the anomalous
behavior
ele. -
of disof Ne,
T
e
or Vz at night.
A very
e“ident
large
oscillation
i“ hmax and electron
in Fig. 6(a) that appears
oscillations
(of appropriate
behavior,
albeit
to be the result
was evident
between midnight
of a long-period
sign) in the electron
less pronounced,
density
temperature
TID.
There
and vertical
on 23-24 3%bruary
and 0600 LT is
are corresponding
velocity.
Similar
[Fig. 8(a)] and 3-4 October
[Fig. 24(a)].
Other recognizable
densities
,
features
(presumably
temperatures
which may he produced
resulting
ever,
from
when overhead
[Fig. 8(b)].
E-region
by particle
precipitation
nocturnal
It is tempting
density
increase
to attribute
increase.
most unusual and probably
indicative
on the basis
temperature
increase
of the layer
above h~laxFZ
The results
no ob”ious
perturbations
turbed winter
attributed
cently
origin.
Based upon observations
there often are large
strong
electric
lifting
A particularly
striking
of 6300-~
equatorward
a clear-cut
that the
sunrise.
Comparing
caused a very
Large expansion
sunrise.
November)
nocturnal
and, in part,
airglow,
While
fields.
of the layer
contain several
temper-zt”re
gaps,
increases,
b“t
are available.
in part,
here,9 these disturbed
disturbed
hy the acceleration
on about 0300 LT probably
pro”ided
ahmg the .mroral
winds can be derived
nighttime
nights near midnight.
cases
from
are of special
These
to the air as it crosses
motion of the ions (at speeds
by heat deposited
sults presented
centered
we re-
was observ?d on 23-24 Mm-cb [Fig. ‘tO(a)]
32
and others ha”e found that
Hernanr3ez and Roble
field-induced
Since neutral
s“cb is often the case,
example
winds on magnetically
cap region.
of several
hun-
owal which expands the
tbe inmberent
interest
scatter
re-
and are tbe subject
study.
Quiet Summer
In summer
the daytime
Unfortunately,
for which good measurements
that long-lived
air in the polar
D.
to be no
peak have been noted previously’
on dis3’t
30
and Park and Meng,
usually ha”e been
the work of Park
of substorm
cap by the rapid electric
of a separate
seen at local
day (15-i6
appears
0600 and 1000 1.T is
and it is possible
with conjugate
increase
on possible
during the periods
winds appear to be caused,
dred meters/second)
winter
conclusions
nights and, following
have recognized
associated
How-
in the height of the layer
to the presence
has a different
the polar
effect
the
on 24 February
since there
here,
from
during 1972.
between
effects.
F-region
seem to have been no
observed
heating,
field
heat fluxes
at Millstone
of the data presented
of the type normally
to draw firm
ones appeared
Large
electric
(’t ) enhanced E-region
There
temperature
of hmax especially
that the temperature
for the other disturbed
making it difficult
was obser”ed
of large
is a predawn
Figs. 8(b) and (d), it is evident
or large
particles.
this to protospheric
association
include:
and (2) enhanced electron
precipitation
in electron
The oscillation
is not possible
behavior
particles)
the decay of ring-current
particle
there was a large
nighttime
by precipitating
plasmasphere
instances
.,
of disturbed
produced
time,
Behavior
tbe electron
density
by an amount that increases
at levels
at sumpot
near h~axF2
maximum.
is lower
than in winter
It now is recognized
during
that this
reflects
a change in the composition
transport
of atomic
oxygen from
The diurnal variation
from
[n the present
havior
data set,
We earlier
behavior
is quite rapid,
electron
exhibits
a much larger
di”pnal
occurring
(Fig. i 1) is the first
near
variation
The switch
within a week or two of equinox.
day to exhibit
tbe quiet summer
be-
to account for tbe evening
increase in Nmax in terms of the contrac%1
when the electron temperature
decreases
at sunset.
33
ion drifts
confirmed that there are indeed large downward
that occurs
of vertical
of the cooling
of the layer.
These
5 x 108 ions/cm2 (Ref. 7).
34 ~“d Kohl et ~1.35
An alternative
explanation for the phenomenon put forth by Kohl and King
——
is tklat it is caused by the reversal
of the meridional
component of the neutral wind. During the
daytime,
to lower
fluxes
is encountered
heating is absent at night.
of the ions above hmax F2 at sunset as a consequence
lead to dowmvard
density
by horizontal
(Fig. 23) the last.
(m- collapse)
Subsequent observations
temperature
as then conjugate
26-27 April
attempted
tion of the layer
drifts
The electron
a“d 12-13 September
introduced
739
hemisphere.
also in that the largest
than winter,
Ilwinterll to ‘rsummer!!
air at these levels
the summer-to-winter
differs
sunset and not near midday.
at Mills tom in swmner
of the neutral
through 650 km at sunset of the order
the wind blows poleward
altitudes
and this acmtmts
where
the recombinatim
earlier
using incoherent
in winter
are higher.
At night,
field direction)
the situation
is reversed
scatter
than summer
observations
~.. --–—T-
and experimental
results supporting this were obtained
36
by Vasseur.
Figure Z7 illustrates
this effect in results
Millstone.
-----m
MILLSTONE
[
(along the magnetic
in the diurnal variation of the F-layer,
especially
in sum34 ~“d Kohl et ~1,35
Kohl and King
proposed that the wind direction
for the neutral air winds obtained from
?,0
rates
the layer
for the smallness
mer when the night is short.
reversed
tending to drive
300
H,,
m
Fig.27.
velocity
Estimates of the rneridi.rml
wind
at 300 km derived from incoherent
scdter
results showing the eorlier reversal
from mrthw.rd
tO southward winds in the
afternoon i“ summer (J .E, Salah,
private
comm.”iccdion).
EST
(br)
98
—-—
.
.-, -
The role of neutral
detection
air winds in generating
of a magnetic
ticm st”dies~9
winds is the more
E.
declination
At this juncture,
Summer
Owing to the shortness
particle
values
below that of the IM.
of atomic
turbed sig”ifimmtly
or < 5(a)].
period
fields
This behavior
may play a role,
appears
disturbed
that of the
peak density
is thought to be caused
by an increase
hemisphere.
an oscillatory
behavior
TIDs tend to be associated
to have been a fairly
re-
than in
sometimes
to
in the rate of
Only one day (30-31 May) was dis-
[Fig. 14(a)]
the presence
behavior
is less often observed
of tbe F2-region
of Vz suggesting
for which the average
in summer,
or heat fluxes
on this day were
hmax exhibited
While these large-scale
heights
is a depression
and the densities
oscillations
There
electric
featwe
oxygen cmt of the summer
In addition,
the case.
both effects
Behavior
precipitation,
The most striking
with associated
that, while
of the night at F-region
winter.
migration
has been confirmed by the
37,38
and computer simulaof the imz-ease
in the size
it appear~
increase
important.
Disturbed
sulting from
effect
an evening
below
between
normal
Figs.
i3(a)
about ~500 and 0300 LT
of large-scale
with magnetic
pmmoumed
[cf.
‘r IDS.
activity,
this is not always
TID on 9-i O May (Fig. ‘f2 ) during
value of the I<p index was only 2+.
Similar
findings
were
a
reported
in Ref. 9.
W.
RESULTS
A.
FOR
AND
FLUXES
General
The signal
mately,
H+ DENSITIES
spectra
are measured
150 km.
Normally,
of the reflections
at interwals
these spectra
0+ is the only ion present.
over
the altitude
interval
45o to 1125 km, approxi-
of 75 km using a pulse that yields
are analyzed
It also is possible
to yield
estimates
to reanalyze
these
a height resolution
of Te and Ti assuming
spectra
to yield
of
that
estimates
of
the H+ percentage
as well as Te and Ti.
‘The computer program
employed for this was written
40
and modified subsequently by R. Julian.
Unfortunately,
the program is slow,
by J. L. Massa
owing to tbe large
search
that must be undertaken,
and thus far this has limited
the number of
days that could be examined.
Early
attempts to use this program were for data gathered
i8,’t9
maximum.
Subsequently, the program was used to reduce
i.e. , nearer
allow
sunspot minimum.
conclusions
tosphere
O“er
to be drawn concerning
results,
implications
a major
B.
,,i
that the results
we discuss
report
of these results
advance
the data reduction
values obtained
for eleveu
o. the nighttime
on a previous
between
to sunspot
in 1972 and 1973,
interest
since they
the ionospbe,.e
to obtain estimates
of the days listed
proto nospheric
study ‘9 whose conclusions
and magne-
fluxes.
were
of H+/Ne from
in Table
incoherent
111, and discuss
the
This last topic represents
not thought to be very
reliable.
Data Reduction
The program
employed
to determine
YSIS and INSCON
programs
used to generate
been used only to examine
program
close
data gatbered
are of great
the proton fluxes
i.e.,
Millstone.
In this section,
scatter
We belie”e
in i969,
is required
the C-mode
to search
the H+ concentration
the results
spectrum
results
for the best fit between
99
._ ... ...——
-.....,m.
,.
is run separately
described
recorded
in Sec. IH.
from the ANALTo date,
on the original
the measured
spectrum
it has
data tape.
The
and the theoretical
spectrum
describing
the scattering
ducted in a library
bks
the Fourier
rather
of calculated
transform
than spectra
is calculated
of tbe measured
facilitates
separately
Crom an 11+/0+
autocorrelation
puter.
Unfortunately,
2
a , where
there
spectrum,
the calculation
and the resulting
ion mixture.
functions
To do this., a search
The matching
of the instrumental
functions
are four variables
are stored
in all,
i~ cOn-
for tbe one that most closely
viz:
of co~relation
effects
(below).
r-esem -
functions
Tbe library
on the drum of the XDS 9300 tom-,
ff+I’Ne,
Te,
‘ri,
and the variable
(%)2
“2=
~
r
in which
[De .6.9
~
(’t)
(2)
cm
e
is the electron
Deb.ye length when Ne is in electrons
‘2‘4)
‘rhe dependence
tion functions.
upon Ti can be eliminated
since it controls
the present
the scale
library
in 0.1 steps
c!
2
= 0.0,
O.O*, 0.025,
0.4i,
difficult
of computing
axis only,
to solve
0.042 0,057,
0,074,
the library
i. (?. Ac-
as @2 -
Over a range Of cases
0.09,
of correla-
and not the shape of the function.
for tbe H+/Ne ratio
has been comp,,ted
u+/h
.
e
0.4
of the time
of spectra
ir 0.2 steps
to
A = 68.18 cm)
(3)
for the purpose
~t becomes
‘~e/’?i = 0.8 to 3.0
0.0
(where
.KCIT13
.
As simw,, by Moorcroft,+l
cordingly,
For Millstone
/cm3.
that includes:
0.17, 0.25, 0.33,
0.49, 0.60
‘Ti . 8oo~K
These
delay
theoretical
autocorrelation
(by parabolic
performed
Tb.
range of H+[Ne
(f325-km nominal
sequent analysis
increasingly
program
I
ceeds
are computed
for points 10 psec apart and scaled
in
at ezcb iteration
to match the actual ion temperature
probably
altitude
height),
was chosen after
an analysis
does not yield
Despite
for the effect
rarely
the library
effects
This
if ever
cases
for
and sampling
could be
Sub-
this rule was
it is believed
that the
where the H+ abundance ex-
can be drawn and no attempt
11+percentage
greater
each experimental
power spectrum
has
than 40 percent.
spectrum
the output of a recei”er
tt,e Doppler-broadened
18, i9,40
40 percent.
sunspot minimum,
for those altitudes
on tbe obsewations,
estimates
exceeded
Accordingly,
useful conclusions
to include
causes
with a function
nights.
results
of gating the trarmznitter
filters.
W(w) to be convolved
reliable
this Iimitatior>.,
To allow for instrumental
of tbe i969 results
for which it was thought that reliable
the 1{+ pert.”tage
at high altit Lldes 0!1 winter
been made to recompute
a bank of matched
ratios
of days in 1972 and 1973 showed that nearer
violated
50 percent.
rected
in order
dw-ing tbe best fit seai-ch.
limited
showed that at the greatest
obta.i”ed
functions
interpolation)
is cor-
containing
of the medium
j(x)
where
sin (xT)]
.~[i–~
nTx
(4)
x . u – u, in which WI is the angular frequenrdv st which the power
the pulse length (1 msec).
formed
and the result
which is simply
La.t to limit
theoretical
To remove
is divided
a triangular
weight
the experimental
tramform
f“mti on.
spectra
Since Eq. (5) tends to zero
effect
This imposes
is the limited
a further
moved and hence it was necessary
duce the same effect.
(at 4O.+sec
range of frequencies
weighting
of the measured
to weight the theoretical
This was accomplished
intervals
function the” wzs Fourier
transformed,
interpolation
weighted
o.er
trans-
sampled
spectra.
by the filter
functions
bank
to repro-
a“tocorrelation
points every
the frequency
and
This cannot be re-
the calculated
to achieve
T, it is impOr -
the measured
autocorrelation
by interpolating
) by parabolic
are Fourier
at T -
over which a matr.h is sought between
40
functions.
A second instrumental
(+i i. s k]lz).
and T is
of Eq. (4) namely,
the range of ~ valws
autocorrelatim
functions
this effect,
by the Fourier
is observed
5 psec.
range of rilter
This
bank by a
weight w(f),
w(f)
and then transformed
deemed
neces~ary
= 1
–i2
.0
elsewhere
Various
from
to a“oid
approaches
(-25
spectrum.
*2 closest
to m~.
expansion
to allow
least squares
lli)’Ne,
and a 2.
such as using the results
.Howanc. e is made for the
mean height to be associated
is conducted
function is expanded
between
one.
for the value of
order
in a Taylor’s
grid points and a linear
sum of the differences
and the theoretical
in the measurements.
to first
ll+/Ne and Te/Ti
the weighted
with each
for a match between
between
This is carried
tbe mea-
out at seven
The weights are chosen to reflect the
40 ,rhi~ proce~~ is repeated to OPtimize
of T..
a solut;on
If tbe wlue
has been obtaimed,
so obtaimd
se+m-cb is conducted
again.
has not changed sufficiently
are encountered
the printout.
‘re/’Ti,
and any of the set calculated
at , = 41.66 psec (1000/24 psec) apart.
ratio
of Ti,
profile,
a search
cl:),
fmcticm
function
than the
best to use the results of the ANALYSIS
2
The “aluc of e can be calculated [via Eq. (3)] and
(e. g.,
to mi”irnize
was
it seems
in the intervals
autocorrelation
of signal-to-noise
the estimate
a2.
calculation
much larger
best guess have been tried
autocorrelation
fit is performed
best guess
and weighted
auto.orrelation
The selected
sured (corrected)
points spaced
the nominal
becomes
5 pec
the points of the function to be
of Ne from tbe ANALYSIS
obtained this estimate
(corrected)
between
an initial
However,
wlue
km) between
Ha”i”g
the measured
After
selecting
this initial
height.
the appropriate
difference
I
involves
to selecting
lower
‘J’he use of points every
when the im temperature
for Te and Ti and set H+/NC = O.
reduction
i. selecting
variation
aliasing
function.
causing the time interval
search
the previous
+12 kl~z
back to an autocorrelation
nominal “alue of 800-K,
,ed”ced,40
‘The computer
< f<
(e. g.,
a:)
The entire
to alter
and for these cases,
the re”ised
now is closer
process
“alue
of Te is used in Eq. (3) to recalculate
to another
is stopped
after
set within the library,
15 iterations
the
or whenever
a!:
the best library set to “se.
Values of LY2greater than 0.6
2
a = 0.6 library is used, and the results are flagged on
“0° -mmL
/
)400 —
lSIS/MILLSTONE COMPARISON
57-DIP LATITUDE
1972
?’:
/
!
/-
1--.
I
..
$ 800
.
,5-==
‘
600
400
0
w
,S, S
1406
LT 6 SEPT 69°W
ISIS1444LT
7 SEPT 79”W
MtU$TONE )431 LT 6 SEPT
0
M+ CONCENTRATION (Pwc@nfb
~~m
,60”
ls!S/MILLSTONE COMPARISON
57° DIP LATITUDE
)972
, 4CQ
I
7
/
LT 7 SEPT O.lOW
M(LLSTONE 0052 LT 7 SEP1
MILLSTONE 0134 LT 7 SEPT
,S, S 0120
/
4—
600
400
—.
I
_——
(b)
2001
1
0.1
0.2
,
,
I I
0.. 06
II
1
/
+
~
/—’
,
2
I I I I,
4
6
L&&
Ill
10
10
20
H+ CONCENTRATION (Dmc.”!]
Fig. 28.
Comparisonsof the percentage obundonce of H+ ions at the dip latitude
of 57” made by Millstone
Hill and the ISIS sotellite
The broken curve is merely intended
cmnm.nicati.
n).
data ,ets can be ccmec ted
by a re.scm.ble continuous
and (b) nighttime.
ioz
(J .H H. ffrnanr private
to suggest that the two
vari.t
ion.
(a) Daytime
C.
Accuracy
It is difficult
on an analysis
to assign
an experimental
of the accuracy
in the incoherent
scatter
spect to altitude
and time.
values
!’
.,
provide
(i. e., the fit between
reliable
such cases,
results
Some confidence
the range of likely
valwes of ‘re,
tkie theoretical
are cases where
and/or suffer
it typically
are outside
with improbable
is thought that these “s”ally
i;
;
values based solely
measurements.
can be gained by examining them for consistency both with re6-9
data
are particularly
useful for such analyses.
It
of the estimates
also are associated
solution
poor
to the H+ percentage
spectrum
The !fdrifts’!
is found that some fractim
points
accuracy
of the experimental
from
Ti,
and experimental
the experirne”tal
one or more
H+/No at a given height is of the order
and these
suggesting
spectra)
spectra
particularly
is fmmd that the root -mean -sq”ai-e
“alues,
and/or Te/Ti
has been found.
simply
It
are too noisy to
bad points.
scatter
that a
Eliminating
of swcessi”e
estimates
of
of +30 percent.
Comparison
has been made with H+/Ne ratios measured wing the mass spectrometer
on
42
1S1S 11 at i400-km altitude
on a few occasions in i972 when there was a pass of the satellite
to the east or west of Millstone
communication).
Since there
lite and Millstone,
of H+ provided
into .3 single
plot.
tended simply
tirmous curve.
are provided
scatter
(John Hoffman,
in the longitudes
private
of the satel-
the “alue for the percentage
(57’)
of Millstone
chosen and an attempt
in Figs. 28(a-b),
that it is possible
Tbe incoherent
difference
by selecting
the dip latitude
time then were
Examples
to suggest
compared
as it crossed
by the satellite
at the same local
also was i“ operation
usually was a significant
the two data sets were
stone values
to
while the radar
where
Hill.
The Mill-
made to combine
the broken curves
the two
are in-
to connect the two data sets by a reasonable
measurement
error
and con-
bars in this plot ha”e heen set equal
*3O percent.
The ISIS results
latitude
of Millstone,
of the incoherent
D.
provided
He+ always
scatter
of H+, He+, and 0+ and appear to show that for the clip
estimates
results
remains
a minor
can be justified
ion so that its neglect
—at least
as a first
in tbe interpretation
approximation.
Results
For the present
study,
eleven
days in 4972 were
25-26 January
analyzed.
12-t3
23-24 February
They were:
July
7-8 August
9-i O May
b-? September
30-31 May
15-t6
S3-14 June
No”ember
6-7 December
30 June – i July
The diurnal
variation
could be obtained
(usually
of H+ percentage
825-km
nominal
pulse lies near 800 km) is shown in Figs.
50 percent,
results
for the next lowest
The diurnal variation
in 1969 were
between
summer
was attributed
time,
publisbed
29(a-k).
altitude
Where
tbe density
weighted
estimates
height of the
at this height exceeded
height are gi”en.
of the H+ percentage
co”ce”tration
18,49
A marked difference
and winter
for which reliable
for which the effecti”e
previously.
days with the latter
to the annual variation
the H+ percentage
at the highest
altitude
exhibiting
in the mea.
at a single
higher
exospheric
at 800 km was found to be quite small
altitude
for four days
in abundance appeared
abu”dzmces.
43
temperate..
to exist
This difference
I)uring
– usually <t percent.
the dayBegitmi”g
io3
,. .—.
.—--
. ... . ....
I+
FLUX
Dow-.+
LOCLL
TIME
I, ST)
(a)
,...–—.—
T --F:T!-Iii&
.,,,,,0.,
,)0
,0
HILL
.4? 1972
mo
h
J
1
{
“i
Fig.29(a-k).
Edim.tes
of the percentage
of H+ ions .ver
404
II
i
Millstone
Hill
v, local time in 1972.
-.
.T..
7—
7
“-
lKmE
MILLSTONE
HILL
MILLSTONE
“,LL
,3-M
,“.,
1972
800 km
30
,“,;;.(
~mLY
1,72
t
LOCAL
TIME
(EST)
(.)
--—7
Lm
TmvmL
.s!>?.
., LLSTONE
.!,,
s,0.,
HILL
12-138 ~kYm1972
HILL
7.:oAfl,~2
,3
,0,.7
.VERAGE1
1
LOCAL
TIME
(h)
Fig.29(a-k).
,,\
,,.,.
.;
I
Continued.
$05
(EsT!
\
1
\
\
,
k
I
\
\
\
\
\
\
\
\
J..
.4
LOCAL
,00 —–...–
......
TIME
1,S11
--—
,0
‘t
, ,1...
,Tl
0.
mu,
TIM,
m
12
,...,
lESTI
TIME
(k)
(i)
F}g,29(a-k).
Continued.
i 06
,.
(SS11
just before
midnight,
cent in winter
vertical
it usually
at 800 km.
profiles
These
of H+ density
H+ flux at Millstone
to sunrise
increased,
this peak value typically
During 1969,
In an effort
small
values
It is clear
over
to test this conclusicm,
additional
of the winter
at 800-km
small throughout
contrast,
between
E.
midnight
altitude.
a period
BY combining
to construct
tbe
then prevailing
behavior
with
the H+ abun-
in Figs. 29(a-k),
which
in 1972.
is approached,
sunrise
analyzed,
would cwse
larger
amounts of H+ can be detected
found in summer
that the flux was still
clearly
remained
upward at all times.
can be identified
By
that persists
(Sec. F).
Profiles
of 11+estimates
to construct
~v
a profile
with the electron
of H+ vs altitude.
I
E\
,0.0
ewm’ise.
io tO 30 Per-
a few hours prior
days in f972 and 4973 were
when the flux is downward
the percentage
it is possible
for perhaps
In $972, the H+ concentration
and ionospheric
H+ Concentration
separately),
made it difficult
was borne out as indicated
and summer
the night and hence it appears
in winter,
ionospheric
and in the range
that at this phase of the sunspot cycle,
temperatures
that as sunspot mi”imun
Millstone
of H+ percentage
both by day and by night except
that the lower exospheric
44,45
dance to be Larger.
This expectation
examples
just before
in summer
nights.
the expectation
provide
a rnaxim”m
a“d tended to suggest
was qmwrd
on some winter
reaching
was <10 percent
I
I
MILLSTONE HILL
30 JuNE 1972
1229-1421 EST
mu
density
profile
Figure
30 provides
I
I
1
(deduced
I
such a
I
A
T,
T
T
P
300
1
*OO
lmEIL
o~
1
,0
I.QIO
Fig.30.
Ti,
of the daytime
cmd T, observed .ver
using data gathered
measurements,
the plasma
smaller
steerable
along and perpendicular
exhibits
over
Hill
variations
system,
to the magnetic
from
a 2-hour
allowing
field.
downward
loco
IYW
2C02
m.
m
am
TEMPERATURE [.K1
Ne,
N(H+),
interval
0+
ion velocity,
near noon on 30 June %972.
meridian
plane was measured
the ion velocity
to be resolved
In Fig. 30, the parallel
to upward 0+ flux above
in Fig. 30 are the electron
and ion temperatures.
root-mean-square
Of the points gathered
scatter
.f
ma
in 1972.
drift in the N-S magnetic
radar
the usual transition
altitude
MiIlstcme
plot constructed
L-band
1
,0
PARALLEL VELOCITY [.1s.,1
(mlcmtrdi.n/cm’1
Example
1
m
Where
plotted,
at each altitude
component
over
using the
into components
is plotted
about 500 km.
the error
Also
bars indicate
the 2-hour
In these
and
shown
tbe
interval.
-. ...—
1
‘“j , , ,,
1.agn
.;
(CmRn,r.,icdm
,IWIITTL
,,,
-mu
?34
I
0+
-.0
-60
MILLSTONE HILL
6-7 DEC1972
0225-9112
EST
-40,-20
0
0
500
Imcolmaxomo?cco=c’
TEMPERATURE(-K )
vERTICAL VELOC!Tt (! WS.C)
(a) Winter.
,000
,00
000
700
MILLSTONE HILL
30-31 MAY 1972
2243-0048
EST
EJ
//
‘,
Ne
—
i
5
:
~
600
:
400
500
300
200
,00
L
H+
1
o~>
Ibglo
I
-30
)
0’
-20
-10
0
10
-EEL
I
I
(mce.lrnlion/cms
~-
20
30
VERTICAL VELOCITY [m/see 1
0
500
lC.W
TEMPERATURE I-K)
(b) Summer.
Fig.31(a-b).
Examples of the nighttime altitude variations of Ne,
Ti, and Te observed over Mi I Istone Hi I I when the H+ fl .x appeared
108
N(H+),
0+ ion velocity,
to be large.
15C0
The H+ profile
ation expected
appears
cycle.
exhibits
a peak value
when the flux is upward and close
tO Prevail
over
Millstone
(We have not examined
that whenever
aPPears
of the behavior
are tmical
of winter
650 km,
tO be near
value that carmot reliably
were
yet the behavior
the velocity
descending.
at exactly
is in the daytime),
is mt constant
the values
from
that is independent
by charge
Some contribution
be small.
Thus,
to this “due
the arriving
cur”e
downward,
may be caused by my descent
H+ flux at this time appears
in
albeit with a
velocity
results.
fn
if the layer
simply
that there is a downward
of altitude.
exchange
value.
plotted
alone.
as would be expected
flux of 0+ ions of 2.i x 108 ions/cm2/sec
created
behaviOr
altitude on this occasion
400 and 600 km suggest
flux implies
that these ions were
The results
the 0+ vertical
at all altitudes
between
This
it is close to its limiting
3i(a-h).
certainly
the H+ abundance
flux can be gathered
Sec. F).
and over most of the sunqwt
The 13+/0+ transition
night conditions.
from
(cf.
of tbe vari -
sunspot minimum. ) In sum, it seems
and hence the H+ ffux is almost
Instead,
value
in all seasons
found at night are shown in Figs.
be estimated
Some idea of the arri”ing
this instance,
to its limiting
during the daytime
the flux is upward (as it always
Examples
Fig. 3i(a)
near 600 to 700 km that is a characteristic
The constancy
of the
with H+ ions at some greater
of the layer,
but probably
height.
this will
to have a value of approximately
2 x 108 ions/cm2/sec.
In Fig. 31(b),
we show an example
centration
exhibits
conclusion
is supported
limit
observed
by the 0+ vertical
velocity
suggesting
results
measurements
as the layer
obtained
near the layer peak is the best estimate
peak).
of the downward
then the escape flux must be -2 x i08 ions/cmz/sec.
This
46
the behavior predicted by Bailey Q ~
from their time-dependent
1970, although the escape flux then was considerably
If the layer
to be descending
“elocity
to be a
(based
that the velocity
of the layer
case seems
This
about 400 km,
This would appear
If it is assumed
whole,
the 13+con-
that the flux is upward.
as the whole appears
near the layer
In this case,
which show that abow
with a value of about 1.2 x 108 ions/cm2/sec.
on the H+ flux escaping
on the velocity
night behavior.
a peak near 650 km and then declines
the 0+ flux is positive
lower
of the summer
as a
quite similar
to
model for 2300 LT in March
smaller.
is decaying rapidly,
then the 0+ flmi may everywhere
be downward, e“en though
46
In this case, the 0+ velocity observed
by the radar will everywhere
be
the H+ flux is upward.
negative.
This is the more usual situation
I
0,
3
log,,
4
(m..,.,
m, ion /cm
5
3 )
,, -,,
encountered
-m -,
0+ PARALLEL
I
0
VELOC!TY
I ~..
!0 15 0 50.
( ./,,,1
and is illustrated
1000 !500
moo
in Fig. 32.
25c0
TEMPERATURE
{-K)
More usual example
of the nighttime
altitude
variations
of Ne, N(H+), 0+ ion velocity,
and T= observed in summer.
Here the H+ flux is thought to be weak (see text).
Fig.32.
Ti,
,
at Millstone,
109
.,
It usually
L-band
radar
me”ts parallel
assumed
.
.
.....
is impossible
to secure
and perpendicular
also becomes
small,
it may be difficdt
stone.
Nevertheless,
F.
oblique-incidence
to the field
by drifts
large
to infer
it usually
vertical
Iim.
parallel
are created
O++
the forward
whether
vertical
velocity
using the
into ,mmpo then mmt
line, and at night the scatter
are weak.
its value [.wm the vertical
can be established
measurements
cannot be resolved
The observed
to the field
when the signals
in the F-region
Thus, if the H+ escape
0+ flux estimates
be
i“ these
flux is
obtained
at Mill.
the flux indeed is upward (Sec. F).
and reverse
equilibrium
the ions are created
is large)
reaction
chiefly
likelihood
rates
and diffuse
some
own.
just above the F2 peak (i. e., where
that can be sustained
H+ production
equations
of continuity
of thermal
gradients.
H+ is a minor
concentration
the Iimiti”g
the 0+ conce”tre.tion
through the neutral
atomic
oxygen
flux
rate.
ion, its concentration
can be found by solving
the coupled
and momentum for 0+ and H+ and allowing for diffusion under the influence
50
Figure 33 illustrates
the essential features of such calculations;
it is
that the H + concentration
In Fig. 33,
distance
to establisb
by the fact that
back to 0+ [“is the reverse
reaction Eq. [6 )].
This
48,49
which is the maximum possible upward flux
escape
for a given
H+ ions are cre-
The upward H+ flux is limited
considerable
of being converted
where
47
upward within the flux tube in an effort
of their
at altitudes
may be found in Banks St ~.
leads to the concept of a limiting
In the region
reaction
(6)
distribution
and then must diffuse
with a finite
by the charge-exchange
HCH++O
ated [via Eq. (6 )] i“ the daytime
a diffusive
evident
drift
velocity
H+ Fluxes
Protons
,
useful
and hence the observed
at night
to be caused entirely
measurements
where
.,_
is quite sen. iti”e
or critical
are shown for values
escape
flux ~p
to the “due
of tbe flux when this is upward.
is i.45 X 407 ions/cm2/sec
of upward flux Gp . 1.0, 0.9,
0.6, 0, –1.0,
a“d
curves
and —3.0 times
,
(
~-—
)f
. . .. ... ..... .
,0,
ION
CO MC EN IR4TION
.—.-L
,0.
,+
L
lkm-3)
Fig.33.
Idealized curves of H_+ and 0+ concentmtion
for various values of the H+ flux.
Here the 0+ flux is zero and Gp is the critical escape flux for H+ (after Geisler49).
Iio
of H+
.. .
this amount.
It can be seen that for zero or downward
found to increase
altitude
[N(O+)
increases
lezs
approaches
F-region
,.
.. _..
approximately
= N(H+)]
is reached.
rapidly,
thereby
the limiting
and remain
fluxes,
as fast as the 0+ ion density
For significant
raising
value,
the H+ comentration
a minor
the H+ concentration
decreases
positive
the t~ansitio”
fluxes,
altitude
initially
is
– until the transition
however,
the H+ density
comiderably.
may exhibit
icm thr-cmghcmtthe region
..,.
AS the escape
flux
a peak in the upper part of the
accessible
to observations
from
Mill-
stone Hill (<1000 km).
The curves
of Fig. 33 were
altitude
1230- K) a“d realistic
will
modify
the role
ever
the distribution
somewhat
– tending to increase
distrib”tio”
is less important
to identify
From
a“d close to its limiting
periods
iomsphere
when the flux over
during the daytime)
T“
the transition
altitude.
than the magnitude
value.
Millstone
49 (Tn = Ti = “r, =
(’re & Ti >
However,
of the flux,
when-
USe can be made of this feature
to
Hill is upwai-d.
Fig. 33 and other more realistic
calculations
conducted by Banks and Kockarts,
52
Rao and Jain,
and others, it appears that a practical guide to the identification
Narasinga
internals
when the flux is large
tude <iOOO km, and therefore
values
at Millstone
the actual test for large
km >20
appear
percent.
a“d downward
is to search
i“ view of tbe radar.
Thus,
800
for M isothermal
of the temperatures
of the tempem.tm-e
this is both positive
attempt
constructed
variations
In practice,
to be obtained near 800 km,
Where
for periods
the most reliable
i.e. , about one scale
are obtained
at higher
of
when the tramition
downward flux has been to find periods
good results
51
alti-
H+ (percent]
height below 1000 km.
when the H+ abundance at
altitudea,
they appear to support
this rule.
From
times
an inspection
o“er
includes
results
spot
V.
minimum
(albeit
DISCUSSION
and time variations,
appear to be present.
for i969 and i973.
It is clear
for shorter
periods,
as a rule,
OF
RESULTS
with Previous
efforts
FOR
mences
at high latitudes
phemxnenon
close
results
have identified
fluxes
a region
and extends over
has been attributed
flux are cow
nights near s.r>-
They always
end shortlj
is approached
FLUXES
of light ions in the upper part of the
haw
been made from
servations
at Arecibo
(e. g., Ho and Moorcroft 53), from &nio.
59-60
*e”t~42,54-58
and from topside electron density profiles.
The & ~
I L,, which
Findings
the concentrations
of exchange
AND
to find tbe
in Table
of dmvmvard
o“ summer
as sunspot minimum
H+ DENSITIES
Experimental
to measure
and infer the presence
that periods
are listed
than in winter).
and appear to begin earlier
THE
we ha”e attempt?d
These
b“t are emmuntered
sunrise,
Comparison
Previously,
F-layer
fluxes
nights near sunspot maximum,
ionospheric
A.
arri”ing
obtained
fined to winter
after
of the H+ vs altitude
which large
of wry
the polar
to the continuous
scatter
low light ion comentratio”
cap (the so-called
escape
incoherent
mass spectrometer
of H+ iom
ob-
measure-
that com-
!Ilight ion trough r’).
at high latitudes
This
at values
to the critical flux along Open field lines (sometimes
called the polar-wind).
Banks and
59
have show” from topside wmnder records that the region of rapid escape extends in
Doupnik
side the plasmas phere
HO a“d Mcmrcroft53
mn2/see)
over
the diurnal
Arecibo.
variation
in the morning
ha”e i“ferred
sector.
the existence
While these values
they observed
of very
seem overly
large
large
on one day is interesting
escape
fluxes
(>i09
in the light of later
as the flw
evidence,
was seen to be upward
and downward
“ear
s“m-ise.
Unfortunately,
was poor and results
were
presented
for only a single
between
2000 and Z400 LT and large
Iutionof
their measurements
4ii
ions/
the time
day.
reso
—
TAB LE IV
PERIODS
WHEN
Dote
Year
1969
5-
February
0200
H+ ARRIVING
Ends
FLUXE!
Comment
b
data above 803 I
0630
9-10
Apri I
23-24
April
%
data above 800
9-1o
July
q.
data above 800
23-24
September
qo dot.
20-21
November
0200
060Q
25-26
January
0200
0700
23-24
Febru.ry
9-10
May
30-31
May
13-14
June
30 June12-13
—
1 July
Juiy
7-
8 August
0300
04CQ
6-
7 September
0200
0400
November
2200
0300
6-
7 December
0000
07C41
2-
3 Jmwary
0200
0600
OCOO
0530
15-16
1973
Begins
BE LARGE
6 February
12-13
1972
THERE APPEAR TO
13-14
February
22-23
May
18-19
July
2300
0403
14-15
August
0200
0400
16-17
October
OOQO
0600
13-14
November
0030
070il
above 800
The most extensive
of Titheridge~O
near solar
study undertaken
who examined
minimum.
tify the transition
siderations
(i. e.,
ignoring
reasonable
agreement
hemisphere
ionization
large
day-to-night
with sunspot cycle.
minimum
spot maximun,
of i973,
any period
B.
Control
heights)
however,
satellite
latitude
the winter
there
in Fig. 35.
This allOWS the
night ionosphere
without in -
is a continuous
appear
for longer
nights,
the fluxes
intervals
of the flu
behavior
on winter
nights as sunspot
are upward throughcmt the night at sun-
flux are encountered
variations
variation
prior
also occur,
to smmise
presumably
as sunspot mini-
in response
to changes
of Millstone
(A . 570 ) at night.
downward
(except
They were,
at lower
howewr,
unable to
latitudes).
of the Diurnal Variations
concluded
that variations
or greater
When the pressure
ions are being created
downward
nighttime
each day,
that the diurnal
the protons
in the ahmdmme
variations
of tbe fluxes
(and hence 0+/11+ transition
and loss of 0+ in the ionosphere.
of neutral
in the topside
atomic
plasma
on the direction
or lost in the F-region.
fluxes,
equilibrium,
variations
by the production
hydrogen
We suggest,
and oxygen
jointly
exert
control.
thus presupposes
6i
are changing
of the reaction
The expectation
only slowly,
Eq. (6 ), i.e.,
dominate
night are replenished.
that this cammt always
be true.
the H+ ion abundance would be given
the direction
on whether
of upward daytime
that the 0+ “xriations
lost during the pt-e”ious
at night demonstrates
exchange
as illustrated
measurements
of H+ abundances during the northern hemisphere
58
also have come to the conclusion that the flux remains up-
of the H+ flux will depend primarily
fluxes
hemisphere
to sustain the tube content.
that there
day-to-day
are caused primarily
comparable
They imply that for much of the night,
and 0+ density.
when the flux became
60
Tit heridge
become
Raitt and Dorling
ward at the magnetic
detect
here.
are summarized
to maintain
of downward
Large
temperature
Using the ESRO-4
summer
On summer
but periods
mum is approached.
in exospheric
but in summer
in Fig. 34 and are in
results
in tube content.
suggest
Downward fluxes
is approached.
con-
that, within the
tht.oughmd the night in winter,
is upward tending
changes
charge-equilibrium
concluded
I
The t ransi -
The8e
that serves
observations
from
Titheridge
to be that
with Alouette
has bee” able to iden
Tithe ridge
with those calculated
with those reported
The flux in summer
appears
gathered
of local time and latitude.
from the flux tube only i“ the winter
flux tube to provide
profiles
to these,
of fl~~es).
are downward
around sunrise.
is a loss of ionization
The Millstone
profiles
compared
the presence
the fluxes
only briefly
density
[ N( H+) . N(o+ ) ] as a function
then were
downward
curring
electron
By fitting theoretical
altitude
tion heights ob’mrved
plasmasphere,
to date of the light ion distribution
60,000 topside
H+
fluxes
and
and that during
The finding of upward
Under conditions
by Eq. (6).
of charge-
The temporal
variation
of H+ ions then will be given by
(7)
i.e. , the relative
three
glected.
It follows
in H together
crease
variation
constituents,
of H+ with time
when variations
that in order
with the percentage
is wmtrcdled
in the temperature
to generate
decrease
by the relative
ratio
Tn/Ti
an upward flux at night,
in O per unit time mwt
variation
i“ the other
(which are small)
tbe percentage
exceed
are neincrease
tbe percentage
de-
in 0+ per unit time.
ii3
.—
-@mm
Fig .34.
Observed
0+
-
H+ transition
heights
at midl otitudes derived by Titheridge60
in 1976
frc.m topside sounder profi Ies: (.) summer and
(b) winter.
Broken lines show the altitudes
puted assuming n. vertical
fl .xes.
Where
observed heights exceed those computed,
comthe
the
f I ux is presumed to be upward.
(b
400
0
,2
6
LOCAL
18
TIME {hrl
NIGHT
m“
SOLST
Fig.35.
Directions
ICE
of the H+ fluxes over most parts of the day and night at solsti.e
(.orfhern
summer).
The diurnal
oxygen
can be inferred
nmdel’2
fore,
I
variation
of 0+ is measured
quite reliably
to estimate
H+ percentage
sureme”ts
baw
has provided
a maximum
at -0400
LT
measmeme.ts
glow measurements,
derived
is in marked
exhihits
“ear
which over the interval
N(H) followed
by a rapid imr-ease
contaminated
in some way by effects
73,74
with theory.
scatter
This same
of the
and such mea.
experiment
can be carried
64-67
of H+ and 0+ abundances
and this
of neutral
measurements
hydrogen
Of N(H+),
an approximately
LT,
to date.
Addi-
observations
N(O+) a]ld N(O),
sinusoidal
“ariation
with
with about a 3:4 diui-md variation
from
some of the Lyman-a
0$00 to 0900 LT indicate
It is possible
at high Iatit”d es,
there-
observations
[Eq. (6)] prevails,
to that inferred
at sunrise.
(such as the MSIS
It is possible,
ha”e been made via satellite
-1700
contrast
imoherent
estimates
from & &
equilibrium,
and a mi”irnum
This variation
from
<t & 63).
the most reliable
concentration
charge -excb’ange
measurements.
equilibrium
of mutr.al hydrogen abundame
airglow intensity. 68-72
of tbe UV Lyman-e
The hydrogen
hydrogen
(Derieux
while that for atomic
of the upper atmosphere
charge-exchange
ion mass-spectrometer
apprOacb probably
(Fig. 36).
where
been made i“ Frame
tional measurements
considering
models
in our experiments,
mass-spectrometer
the abundance of neutral
at tbe le”el
out using & &
more
from
) that are based upon & ~
directly
a predawn
that the airglow
as the simple
air-
depression
in
measurements
sinusoidal
variation
are
seems
consistent
“r-”
-—~”
—
.—
.,,,,
————
.-
!5
“-
~
~iR:=””
. . . MANGE(19731
EXTREME
THEORETICAL
“ALUES
(Tlnste
1975)
[
/, -—---/
.
,0
‘\
.. ___./-
,
~L-~.
. . ........J _-—&J
,0.,.
Fig .36.
The
,etic=l
diurnal
variation
~tudie~,63,73-76
temperature
changes
charge-exchange
According
altitudes
Diurnal
vwicdion
of neutral
lt appears
alone,
,hr)
hydrogen according
that a 3:1 variation
is larger
the influence
with 0+ and thermospheric
neutral winds.
62
O and H have comparable
tbe right causing
These
upward fluxes
charge-exchange
variations
throughout
sources.
equilibrium
64,70,74
of a “umber
than expected
on the distribution
to the MSIS model,
in antiphase.
to several
has heen tbe subject
hydrogen
and may reflect
(400 to 500 km) where
are almost
of neutral
,1.,
diurnal
as a result
amplitude
to force
most of the night in summer.
tbeo of
brought about by
would be expected
appear to be sufficient
of recent
“ariations
to prevail,
Eq. (6) to proceed
at
but
to
In the MSIS model,
mum “ear
concert
0200 LT.
winter
in
its maximum
following
near 0400 LT while
about 0300 LT,
These
may be only a short period
when sunrise
findings
serve
maximum
well
discussed
in Sec. III-FL
after
Comparison
c.
is later,
to explain
rnid”ight,
In midsummer,
why the downward
sunrise
flux from
occurs
near
to be downward,
of downward
flux.
the magnetosphere
of the increase
will act in
in the winter
i-caches
its
night ionosphere
Models
have investigated
theoretical
shouId be a period
its mini-
always
when the flux can be expected
always
and hence the timing
with Theoretical
A number of authors
sphe?e from
there
N(O) reaches
the O and H variations
with that of 0+ to cause the flux to be downward.
0300 and hence there
but
N(H) reaches
Thus,
consideration,
the coupling
between
the ionosphere
s. In the most comprehensive
and protono -
trwatme.ds,
the
ionosphere-
protonosphere
has been modeled as a single unit whose time-dependent
behavior has been simu~ated40,46,61,77 -80
I% avoid a cQmplete solution for tbe behavior of the F-layer
(i. e., including
production,
region
be
10ss, winds,
to be simulated
assumed
to premil.
tbe 0+ density
field
line.
behavior
and electric
fields),
near 400 km where
O“e then may appeal
and temperature
For this reason,
field
“’j
)
and there
when (it is assumed)
aPPIY tOtallY as the conjugate
i
In
by adopting
by static
conditions
to establish
along the
out to simulate
the
has forced
many authors to treat only the
along the two halves
78.9 ‘W) lies at a very
of the field line are identical
this conditim
high southerly
might never
latitude,
where
considerably.
by Marubashi
diffusive
boundary
and Grebowsky,
conditions
These
equilibrium.
f 9701 and showed
(March
measurements
In the case of Millstone,
point (70.7 ‘S,
additional
for the
H+ a“d 0+ can
of the temperature
ha”e been carried
bi
an attempt was made to avoid this
at 3000 km altitude.
was set equal to the rate of change of tube content above,
governed
mum
condition
behavior
fluxes.
may differ
the study conducted
difficulty
level
conditions
scatter
boundary
between
(L . 3.2).
are no interhemispheric
the ionospheric
to adopt a lower
equilibrium
and the variation
a number of the above studies
along the Millstone
condition
to incoherent
at the boundary
The need to adopt an upper boundary
equinox
it is convenient
charge-exch’dnge
calculations
that ward
fluxes
‘rbe
assuming
were
conducted
Of -5-7
flux through this
that the distribution
is
for sunspot maxi-
x ~137iOns/cm2/sec
are ‘0
be expected during the daytime,
i.e., in agreement with tbe observations
we have reported pre6~
18
concluded that the nighttime flux becomes downward at
“iously.
Marubasbi and Grebowsky
sunset and increases
in magnitude
in these calculations,
the atomic
to a peak of -1.5
oxygen
x i08 ions/cm2/sec
abundance zt 500 km was take”
just prior
from
to sunrise.
the CIRA
1972
model and tbe diurnal “ariation of neutral hydrogen waa modeled on tbe results of Brinton
~ay,j4
These variations,
however,
were not large enough to offset the diurnal “ariation
and thereby
effects
the [lUX upward in tbe evening
of the variations
the coupling
In contrast
ewni”g
maintain
between
in 0+,
hours.
O, and 11 at the lower
This
boundary
suggests
and
in 0+
that the competing
make it quite difficult
to model
the ionosphere
to that study,
bo. rs at Millstone
Bailey
a“d pi-otommpht!re mless “cry precise “alues are available.
46
@ &
ha”e found that upward fluxes of 11+can persist into the
based “po”
calculations
employing
different
i’16
—
lower
boundary
“al”es.
ACKNOWLEfEMENTS
We are grateful to R, H. Wand, W. A. Reid, L. B. Hanson and ofhers
at the Millstone Hill observatory who assisted with tie gathering of
the data repxted here, and to R. Julian and Mrs. Alice Freeman
who helped with the data reduction. Dr. J. H. Hoffman kindly PxOvided the LSJSdata shown in Figs. 28(a-b), and helpful comments on
sec. IV were provided by Professor R. J. Moffett. The work was
suppmted by the Atmospheric Science Section of the National Science Foundation under Grant No. ATM 75-22193.
REFERENCES
1. J.V. Evans, “Ionospheric Sackscatter Observations at Millstone Hill,” Technical
Rekwrt 374, Lincoln Laimratory, M. LT. (22 January 1965), DDC AD-616607.
2.
“MiUstone HiJf Thomson Scatter Results for 1964? Technical Re!mrt 430, f&coln Lakaratory, M. LT. (15 f40vemker 1967), DDC AD-668436.
3.
“Millstone Hill Thomson Scatter Resutts for 1965,“ Technical Report 474, iincofn Latmratory, M. L T. (18 Decemker 1969), DDC AD-707501.
4.
, “Millstone Hill Thomson Scatter Resufts for 1966; Technical Report 481, Lincofn Laboratory, M. L T. (15 December 1970), DDC AD-725742.
5.
~rt
, “Millstone Hill Thomson Scatter Results for 1967; Technical Re482, Lincofn Lalmratory, M. LT. (22 July 1971), DDC AD-735727.
, “MiUstone Hill Thomson Scatter Results for 1968: Technical Re6. _
port 499, Lincoln Laiwratory, M. I. T. (23 January 1973), DDC AD-76.7251/2.
7,
I
1
, ‘qMillstone Hill Thomson Scatter Results for 1969; Technical Report 513, Lincoln Lalmratory, M. I. T. (23 July 1974), DDC AD-AO08505/O.
8. J, V. Evans and J. M. Holt, “Millstone Hill Thomson Scatter Results for 1970;
Technical Report 522, Lincoln Labmatory, M. I. T. (11 May 1976).
9. J. V. Evans, B.A. Emery. and J. M. Holt, “Millstone Hill Thomson Scatter Results for 1971,“ Technical Report 528, Lincoln La fxmatory, M, L T.
(24 March 1978).
10. J, V. Evans, Planet. Space Sci. ~,
11,
12.
, J. Geophys. Res. ~,
1031 (1965), DDC AD-616607.
1175 (1965), DDC AD-61431O.
. Planet. Space Sci. Q,
1387 (1967).
13.
, Planet. Space Sci. N,
1225 (1970), DDC AD-716 fJ56.
14.
, J. Atmos. Terr.
15.
—
PIIyS. ~,
, J. Geophys. Res. ~,
DDC AD-714446, respectively.
16. —,
Planet. Space Sci. ~,
1629 (1970), DDC AD-716057.
4803 and 4815 (1970), DD’J AD-714447 md
763 (1973), DDC AD-772 137/6.
17.
, J. Afnms. Terr.
18.
, Plamf. Space Sci. ~,
1461 (1975).
Planet. Space Sci. ~,
1611 (1975).
19. _,
Pbys. 3&, 593 (1973), DDC AD-77187718.
20. J. V. Evans, R.F. Julian, and W, A, Reid, “incoherent Scatter Measurements of
F-Region Densify, Temperatures, and Vertical Velocity at Millstone Hill,”
Technical Report 47’7, Lincoln Lakrmatory, M. L T. (6 February 1970),
DDC AD-706863.
21. G. W. tlrmistead,
J. V. Evans, and W. A. Reid, Radio Sci. ~, 153 (1972)
4<7
—., ~.,,. ,..,..
, :.:.-
-
22.
W. L. Oliver, J. E. L&h, R. H. Wand, and J. V. Evans, “incoherent Scatter Measurements of E- md F-Region Density, Temperatwes,
and Collision Frequency
at Millstone Hill,” Technical Report S31, Lincofn Laboratory,
M. 1. T. (in
preparation).
Wand, .and J. V. Evas.
23.
J. E, sdah,
24,
J, C. Ghilcmi, editor,
‘,Millstone Hill Radar
Technical
Report S07, Lincoln Laboratory,
DDC AD-77 S140.
25.
K, Bibl and B. W. Reinsicb,
R.H.
26.
V. W. J.H. Kirchhoff
27.
J, V. Evans,
Res.
]. Geophys.
28.
G. W. l%lss,
J. V. Evans,
surements:
Res.
30.
CC.
Park,
31.
cC.
Park and C. I. Meng, J. Geophys.
32.
G. Hernandez
“ThermospheTic
paper presented
J, Geophys.
Res.
~,
H. Kohl, J. W. King, and D. Eccles,
36. G. Vasseur, J. Atmos. Terr.
,.,
I
ilys.
1o45 (1967).
1733 (1968).
J. Atmos. Terr.
phys. M,
451 (1971).
J. Atmos.
phy$. ~.
1371 (1971).
and H. M.llmey,
D. Eccles
41.
D. R. MoorCroft,
42.
J. H. Hoffman, W. H. Dodscm,
Res. ~, 4246 (1974).
46.
L9,
MYS. ~>
J.W. King. and H. Kohl,
J. AtmOs. Terr.
J. Ge.phys.
J. V. Evans,
Res.
Terr.
phys.
X.
1927 (1973).
Studies of the tonizatio?
Exchange
PbD Thesis,
University
of Michig=,
6% 955 (1964).
C. R, Lippincott,
D. Alcayde,
and M. Nicolet,
5173 (1976).
J. Atmos. Terr.
J. L. Massa, “Theoretical
and Experimental
Oetween the Ionosphere and Plasma sphere,”
Ann Arbor, Michigan (1974).
J. E. Salah,
8326 (1971) and C8> 3828 (1973).
11, 397 (1969).
40,
G. Kockarts
and H. O. Hammick,
and p. Muer,
AIUI. Geophys.
Ann. GeOphys.
!!> 269 (1962).
, Arm. Geophys.
1>, 370 (1963).
and J. A. Murphy,
J. AtmOs. Terr.
G. J. Bailey,
R.J. Moffett,
47.
P.M.
A. F. Nagy, and W. L Axford,
48.
W. B. klanson
and T. N. L. Patterson,
49.
J. E. Geisler,
J. Geophys.
50.
R. W. Schunkand J. C. G. Walker, Planet. SPace Sci. E,
Fanks,
27.37 (1976).
DDC AD-731927.
Terr.
:39.
43.
~,
RCS. U,
fiYs.
45.
I
Res.
Radio Sci. 6, 609 (1971),
35.
44.
Q,
4650 (1971).
R.G. Roble, J. Geophys.
and J. D. Burge,
Res.
&?, 1635 (1977).
H. Kohl and J. W. King, J. Atmos.
37. M.D. P.pagiamis
J. Geopbys.
Properties
as Deduced from Incoherent Scatter Meam COSPAR Meeting,
Innsbruck,
Austria (June 1978).
34.
:38. D. Eccles,
519 (1978).
4331 (1965).
29.
:33. J. V. Evans,
I
~,
l!?-, 347 (1975).
Sci.
Propagation
Study: !mstrument.tion;
M. I. T, (20 September
1973),
Radio SCi. M,
and L.,A, Carpenter,
J. Geophys.
ad
Radio
Res.
Planet.
Planet.
~,
97 (1976).
~,
1053 (1971).
979 (1964).
Z?, 81 (1967).
535 (1970).
51. P.M. Banks and G. Kockarts, Aeronomy Part B (Academic Press,
52.
~,
PbYs. &9, 105 (1977).
Space Sci.
Space Sci.
J, Geophys.
New York,
1973).
B. C. Narasinga Rao and V. C. Jain, fnd. J. Radio and Space Phys. >, 284 (1974).
53. M. C. Ho and D. R. Moorcroft,
54. H. A. Taylor,
Jr.,
Planet.
, ], Geophys.
55.
56.
H.A. Taylor,
Jr.
pl~et.
SPace Sci. ~
1431 md 1441 (1971).
SPaCe Sci. 2!2, 1S93 (1972).
Re..
and W.J. Walsh,
57.
J. M. Gre!mwsky,
58.
w.J.
Raitt and E. B. ~rfing,
A. J. Chen,
59.
P.M.
Rinks and J. R. Doupnik,
Q
31S (1973).
J. G@ Phys. Res. 17, 6716 (1972).
and H. A. Taylor,
J. Atmos.
Planet.
Terr.
SPa.e
Jr.,
J. Geophys.
pbYs. N,
Sci. ~,
Res.
1077 (1976).
79 (1974).
&l,
690 (1976).
60.
J. E. Titheridge,
Planet.
Space Sci. ~,
and J. M. Gre!mwsky,
61.
K. Marubashi
62,
A, E, Hedin, C. A. Reber, G. P, Newton, N. W. Spencer, H. C. Brinton, H.G. May.,
and W. E. Potfer, J. Geophys. Res. &, 2148 (1977).
63. A. Derieux, P. Bauer,
64.
H.C.
&into”
E, L. Oreig, W. B. Hanson,
26?7 (1976).
68.
A. Vidal-Madjar,
J. E. Blamont,
and 19, 233 (1974).
69,
J. L. Sertaux,
821 (1976).
70.
P, R. Meier
71.
G. E. Thomas
72.
C. Emerich,
J. Geophys.
and P. Mange,
L. Wallace
~,
Planet.
Ann. Geophys.
Jr.,
Planet.
~,
Planet.
H.G. Mayr, E.G. Fontheim,
L. H. Brace,
J. Atmos, Terr. Phys. ~,
1659 (1972).
G.J.
Bailey,
Space Sci. %,
18,
Terr.
1115 (1973)
Phys. ~,
303 (1976).
J. Geophys. Res. 3J, 6103 (1976).
Space Sci. LO, 521 (1972).
LO, 375 (1974).
lWmks, J. Geophys.
and J. A. Murphy>
Res.
&
686 (1973).
78.
R.]. Moffett
J. Geophys.
Res.
626 (1975).
A.F.
J. A. Murphy,
J. Geophys.
309 (1973).
J. A. Quessette,
80.
Lett. ~, 389 (1975).
Space Sci. 21,
76.
79.
Res.
also J. At,mos.
77.
Nagy and P.M.
751 (19’72).
639 (1975);
Planet. Space S,Ci. U,
and D. F. Strohel,
447 (1975).
and D. C. Kayser,
and J. E. Blamont,
Res.
U,
Geophys.
and B. Phissamy,
and D. E. Anderson,
S. Cazes,
, J. Geophys.
75,
J. H. Hoffman,
Res.
&l, 1700 (1976).
Z& 6198 (1971).
~,
and W. E. Potter,
67,
74.
i
R...
, Space Res.
H.G. Mayr,
H. c. wnton,
Res.
Ann. Geophys.
J. Geophys.
66.
73. IL A. Timley,
!
J. Geophys.
and A. Lejeune,
and H.G. May.,
65.
‘1
229 (1976).
PIanet.
Res.
~,
H. C. Brinton,
Space Sci.
and R. J. Moffett,
4277 (1972).
24,
J. Atmos.
and H.A.
Taylor, Jr.,
43 (1973).
Terr,
Phys,
~,
351 (1976).
APPENDIX
INsCON
SUMMARY
1 JANUARY
1979
INSCON
DATE
?5-26,
JAK,1972
25-26,.
JAN,1972
25-26,
J,9h,1972
E’5-26,.!Ati,1972
25v26,.IAh,1972
25-26,
JA!Y,1Y72
25-26,0
Ati,1972
26-27,
JAN, 1972
23-2+,
23-24,
23-24,
23-24,
06-07,1+
FEa,1972
FE B,1972
FE B,1972
FEEi,1972
AR,1972
06-07 .KAR,1972
06-07 >KAR,1972
06-07,
KAR> 1972
C5-10, MAR, 1972
09-10,
MAR, 1972
o9-10)MAR,1972
09-10,
HARJ 1972
09-10,
F!AR,1972
09-10,14
AR,1972
09-10 JFAR,1972
17-18,
MA
R,1972
17-18,
VAR,1972
17-18 >YA%,1972
17-18,
t+AR,1972
17-18,
KAR,1972
17-18,
Y.AR,1972
17-18,
PIAR,1972
SUMMARY,
TYPE
DENsITY
ELECTR8k
TEMPERATURE
10N TEMPERATURE
VERTICAL
l~h
ERIFT
EL EC TROF. TEPPERAIbRL
ION TEMPERATURE
vERTICAL
ION DRIFT
CENSITY
ELECTRON
TF,YPERATu RE.
iON TEMPERATURE
VEBTICAL
IDh DRIFT
ELEc TRO’h lEHPERATuRL
ION TEMPERATURE
VERTICAL
ION URIFT
CENS[TY
ELEcTROk
TKMPERATURL
ION TEYPEEATURE
vERTICAL
ION ORIFT
ELECTWN
TENPERATURL
ION TEtiPEEATUiiE
VERTICAL
[ON cRi FT
DENSITY
ELEcTRON
TEiIPERATURE
10N TEMPERATuRE
vE@TICAL
10N ORIFT
DENSITY
ELECTRON
TEMPERATURE
ION TEMPERATuRE
VERTICAL
ION ORIFT
ELEc TRoh T& KPERATURE
10N TEMPERATuRE
VERTICAL
10K CRIFT
DENS; TY
ELEcTRON
TEMPERATuRE
ION TEMPERATURE
VERTICAL
ION CRIFT
ELEcTRON
TEMPERATURE
ION TEMPERATuRE
VERTICAL
IKih ORIFT
RET IAS
KLTIAS
RETIA5
RETIA3
RET I AS
RETIAS
RET IAS
L/LHF
L/uHF
L/iJb+F
L/LHF
L/bHF
L/bhF
L/bl+F
KET IAS
RETIAS
RET IAS
RET IAS
RET IAS
RET IAs
WTIA5
STATS
STATS
STATS
STATS
RETIAS
RKTIAS
RETIAS
RET I AS
RETIAS
RETIAS
RET IAS
STATS
STATS
STATS
STATS
STATS
STATS
STATS
01, JAN,
1979
START
END
(EST)
(EST)
~242
~z42
~z42
1155
1155
1155
1155
1155
1155
1155
lj947
~947
~947
~9+7
0947
lj947
09+7
1816
1816
i816
i816
0957
0957
0957
0957
0957
0957
9957
1720
1720
172c
1720
1720
172c
1720
1248
1?48
1248
1248
1248
1?48
1248
1440
1440
144G
144G
144ti
1*4C
144G
1153
1153
1153
1153
1153
1152
1153
0631
c&31
0631
0631
1141
1141
11+1
1141
1141
1141
1141
2341
2341
2341
2341
2341
2341
2341
TEST VALUE
.52706E
01
-.94533E
03
-.7279~E
03
-,z5701E
33
-.9455&E
03
03
-,728G2E
-.2571c
E :3
.52775E
cl
-.89529E
;3
-.70(J4~E
-.26(J46E
-,89560
-,69959[
..26027E
,53322E
-,97605E
‘,71946E
-,24834E
-.97630E
‘,7194&E
-,24863E
-.38059E
-,78291E
-,7173GE
-,23727E
,541)5~E
-,78232E
..74757E
-,22471E
‘.7825CE
-,7455(3E
-,22469E
-.44876E
-,8878z
-,75744E
-,25864E
-,88419E
-,7~663E
‘.25893E
G3
C,3
E 03
03
03
01
03
03
03
03
03
93
01
C3
03
03
“1
03
G3
03
03
03
03
01
E 03
C3
03
03
03
03
KDAT
FIT NO.
101
203
3C3
1001
293
393
1C91
101
203
303
72c250
72c250
72C250
72c25G
72c2’50
72c?50
72c?5c
72c26G
72c26C
7?c26c
72c26G
72c26L
72c260
72c%60
72054c
72054G
72C540
72c540
72C54C
72G540
72c54c
72 C66C
72c66C
72c66G
72c66$
72c69c
72C690
72c69C
72c690
72C690
72069G
720690
72c77c
72c77G
720770
72c77c
72c770
72c77G
72C770
1001
293
393
1091
101
203
303
1001
293
393
1991
101
203
303
1091
lC1
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
INSCON
TYPE
DATE
23. Z4, YAR, 197?
23-24,
!’AR, 1972
23~a4,V&R,
1972
23-24,
PAR, 1972
23-24,
wAR, 1972
23-24,
P!AR, 1972
23-24,
MAR, 1972
13-14,
APR,1972
13-14,
APR,1972
13-14,
A!2R,1972
13-14,
APR,1972
13-14 .AFR,1972
13-14,
APR,1972
13-14,
A? R,1972
26.27,
APR, 1972
26.2?,
AQU,1972
26.27,
APR,1972
26-27,
APR,1972
26-27,
ApR,1972
26 T27, ApR,1972
26-27,
AQR,1972
09.10,
MAY, 1972
G9.10,
I4AY,1972
09-10,
F!AY,1972
09-10,
P.AY, i972
C9-10,
MAY,1972
09-10,
MAY#1972
09-10,
MAY, 1972
25-26,
MA Y,1972
25.26,
i+AY,1972
25-26,
25-26,
25-26,
25-26,
25- Z6,
30-31,
30.31,
30-81,
30-3i,
30-31,
30-318
30-31,
KiY> 1972
m4Y,1972
n&Yo 1972
EAY,1972
tiAY,1972
vAY,1972
M8Y,1972
vAY,1972
M@Y>1972
FAY,1972
N4Y,1972
NAY,1972
08-09,
JUN,1972
08-09,
JUN,1972
08- b9, JuN,1972
SUMMARY.
CEN51TY
CLECTRbN
TEMPERATuRE
ION TEMPERATuRE
VERTICAL
IOh-CRIFT
&LECTRON
TEMPERATuRE
ION TEMPER ATLRK
VE8TICAL
10b ORIFT
BENs ITY
ELECTFiOk
TEMPERATuRE
ION TEMPEC?8TbRE
VERTICAL
10N DRIFT
ELECTRON
TEMPERATuRE
ION TEMPERATuRE
;:~:;T;L
ION ORIFT
cLccTRoh
TEMPERATuRE
ION TEMP&BATbRE
YERTICAL
IDh CRIFT
<4 ECTRON TEMPERATuRE
ION TEMPERATuRE
::~:;:;L
[ON ORIFT
ELECTRON
TEMPEI?ATuRc
ION TEMPERATuRE
YERTI CAL
tOtY ORIFT
ELECTRON
TEMPERATuRE
ION TEMPERATURE
VERTICAL
!oh DRIFT
DENsITY
ELECTRON
TWPERATURE
ION TEHPEEATLRE
0f8ricAL
10 N” ORIFT
ELECTRON
TEMPERATuRE
10N TEMPERATURE
YERTICAL
IOh ORIFT
~ENSITY
CLECTRON
TEMPERATuRE
ION TEMPERATURE
VERTICAL
IOK ORIFT
ELECTROh
TEMPERATuRE
ION TEMPERATURE
VEFi TICAL
loN ORIFT
DENsITY
LLECTROk
TEPPERATuR:
JON TEMPERATURE
L/L, HF
L/LHF
L/LhF
L/LHF
L/LHF
L/LhF
L/LHF
STATS
STATS
STATS
STATS
STATS
STATS
STATS
RETIAS
RETIAS
RETIAS
RETIAS
RETIAS
RET IAS
RET\AS
RETIAS
RETIAS
RETIAS
RETIAS
RETIAS
RETIAS
RETIAS
STATS
STATS
STATS
STATS
STATS
STA?S
STATS
L/iJHF
L/UHF
L/LUF
L/bHF
L/bHF
L/bHF
L/IJHF
STATS
STATS
STATS
01, JAN,
1979 (Continued)
START
(EST)
END
(EST)
1619
1619
1619
1619
1619
1619
1619
2111
2111
2111
2111
2111
2111
2111
1604
1604
1604
1604
1604
1604
1604
1231
1231
161L
1610
1610
1610
161C
1610
1610
0559
0559
0559
0559
0559
0559
0559
1701
1701
1701
1701
1701
1701
17C1
1314
1314
1314
1314
1314
1314
1314
13C3
1303
1303
1303
1303
1303
1303
1015
1’215
1015
1015
1015
1015
1015
1714
1714
1714
1231
1231
1231
1231
1231
1136
1136
1136
1136
1136
1136
1136
0922
0922
0922
0922
0922
0922
0922
1023
1023
1023
TEST VALUE
KDAT
050609E
.,90862E
-074096E
‘.26377E
.,90832E
.,74021E
.,26416E
-030205E
-,6992EE
..65812E
-,25724E
-.69700E
-.65660E
-,257o2E
.57314E
U1
C3
03
03
03
03
03
01
03
03
03
03
03
03
ol
‘.1 OO56E
-.73898E
-.27774E
-.1 OO49E
-,73778E
-.27782E
.54065E
04
93
33
04
03
03
ol
-.l
L2g3E
..76517E
04
03
‘.28894E
03
-011291E
c4
-.76424E
03
-.28904E
cj3
.53280
E 01
-.11286E
04
-.73123E
03
-029003E
03
‘.11322E
04
-.73194E
03
-.28994E
03
-.539o7E
01
-o I0966E
04
‘07021;
E 03
..27415E
03
.,10962E
04
-,69988E
G3
-,27410E
03
-,54471E
ol
-,10252E
04
-.73511E
03
101
203
303
10C1
293
393
1091
101
2c3
303
10C1
?93
393
1091
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1’391
101
203
303
FIT NO.
7?c830
72C830
72c830
72c830
7?C830
720830
72c830
721040
721040
721040
72104o
721040
72$040
721040
721170
721170
721170
721170
721170
721170
721170
721300
721300
721300
721300
721300
721300
721300
72146Q
721460
721460
721460
721460
721460
721460
72151c
72151C
721510
721510
721510
721510
721510
72160c
721600
7216C0
INSCON
TYPE
DATE
C8-09,
JUN,1972
13-14 >JUN,1972
13-1+,
JUN,197?
13-1’+,
JUN. 1972
13-14,
JuN,1972
13-14,
JIJN,1972
.
.
.
30
30
30
30
30
JUh-01JLL,1972
JUh. ClJUL,1972
Juk.01JLL,1972
JUN. C1JUL,1972
Juh-Cl
JUL,1972
30 JuP. -O1JLJL,1972
lo-I1,
JuL,1972
lo-ll,
JuL,1972
lo-ll,
JUL,1972
10-11,
JLIL,1972
10-11,
JUL,1972
lo-ll,
JuL,1972
lo-ll,
JuL,1972
12-13,
&L,1972
12.13,
JuL,1972
12-13,
JUL,1972
12-13,
JuL,1972
12-13,
JuL,1972
26-27,
JuL,1972
26-27,
JUL,1972
26-27,
JUL,1972
26-27,
JUL,1972
26-27,
JUL,1972
?6-,27,
JuL,1972
26-&’7,
;UL,1972
37-08,
AuG,1972
SUMMARY.
VERTICAL
ION
ORIFT
ELEcTRON
TEMPERATURE
ION TEMPERATURE
VERTICAL
ION ORIFT
OENSITY
cLEc TROh TEMPERATuRE
ION TEMPERATuRE
VERTICAL
ION DRIFT
EL EcTROh
TEMPERATuRE
~ON TE,IIPERATURE
VERTICAL
IUk ORIFT
PENSITY
ELECTRON
TEMPERATuRE
ION TEMPERATURE
VERTICAL
IOh DRIFT
ELECTRON
TEMPERATURE
ION TEMPERATuRE
VEli TICAL
IL3k ORIFT
OENSITY
ELECTR3N
TEMPERATuRE
ION TEMPERATuRE
VERTICAL
ION DRIFT
ELECTRO~
TEMPERATuRE
ION TEMFERATbRE
VERTICAL
lUi
DRIFT
DENSITY
CLECTR3N
TEMPERATuRE
10N TEMPERATtiRE
VERTICAL
IB~ DRIFT
ELECTRON
TEi%PERATuRE
ION TEMPEBATLRE
W;j]C:L
IOh CRf FT
ELECTRON
TEMPERATuRE
ION TEtiPEBATLRE
ELEcTRON
TEPPERATuR[.
ION TEMPERATURE
STATS
STATS
STATS
STATS
RET IAS
RETIAS
RET[A3
RETIAS
RET IAS
RETIAS
RETIAS
L/uHF
L/WIF
L/bHF
L/bHF
L/uHF
L/uHF
L/LhF
L/LHF
L/bHF
L/LHF
L/LHF
L/LHF
L/LHF
L/L, hF
RETIAS
RETIAS
RETIAS
RETIAS
RETIAS
RETIAS
RET IAS
RETIAS
RETIAS
R~T I AS
RET IAS
RET IAS
L/bHF
L/LHF
L/bHF
L/LtiF
L/LHF
L/LHF
L/bHF
RETIA3
01, JAN,
1979 (Continued)
START
END
(EST)
(EST)
1023
1023
1023
~023
0914
:1914
,0914
C914
a91+
0914
6914
1336
1036
1036
1036
1336
1036
1036
1148
1148
11+8
1148
1148
1148
~148
1208
1208
1208
1208
1208
1208
1208
0840
0840
~8+G
o,34Cj
0840
1029
102.9
1029
1029
1029
1029
1029
0929
1714
1714
1714
1714
1c56
1G56
1?56
1c56
1056
1056
1056
0505
0505
0505
0’505
0505
0505
0505
1Z2G3
1203
1?63
1203
1203
1203
1203
1921
1921
1921
1921
1921
1921
1921
1034
1034
1934
1C34
1034
1409
1409
140Y
i4~9
1409
1405
1409
1106
TEST VALUE
-.23595E
-----—
-073346E
.,23606E
-.54611E
‘.89208E
-,70065E
-.281@7E
-.89161E
-,69914E
-.28095E
‘.53018E
-,11319E
..7026.3E
-.31155E
-,lj308E
-,70051E
-.31152E
.54613E
‘.11674E
-,72147E
-,279I7E
‘.11671E
‘.72129E
-,27919E
-,54054E
-.115c19E
-.73532E
-.27354E
‘.115+2E
-,73510
‘s27230E
‘.52426E
-.98585E
‘,62273E
-,98077E
‘.61538E
‘.543G4E
‘.11463E
-,727o7E
‘,z7342E
-.11477E
-.72617E
-.27354E
.,53095E
KDAT
03
63
03
01
03
03
G3
03
c,3
04
03
03
01
04
03
03
04
03
03
01
O+
03
C3
04
E 03
03
01
03
03
03
03
01
04
03
03
04
03
03
01
1001
i9i
1091
101
2C3
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
2L3
303
293
393
101
203
303
1001
293
393
lrJ91
101
FIT NO.
721600
7216c0
721600
7216c0
721656
721650
72165G
72165c
72166G
72166c
721660
72180G
721800
721800
721800
721800
721800
721~Gti
72182C
72182c
72182G
7?182G
72182Q
721820
721820
721910
721910
72 I91o
72191c
72191C
72i91c
721910
7219$0
721940
721940
7?1940
7219+C
722G8C
7?2c80
722C80
722G80
722080
722o8O
722c8O
722200
INSCON
SUMMARY.
01, JAN,
1979 (Continued)
START
07- C18, AUG,1972
C7-08.
AUG,1972
07.08,
AuG,1972
c7-08,
AuG,1972
07-(18,
AUG,1972
07-08,
AUG,1972
06-07,
sEP,1972
06-07,
SEP,1972
06-Q7,
SEP,1972
06- Q7, SEP,1972
06-07,
SEP,1972
06-07,
sEP,1972
06.07,
SEP,1972
12-13,
sEP,1972
12-13,
SEP,1972
12-13,
SEP,1972
12-13,
SEP,1972
12-13,
SEP,1972
12-13,
SEP,1972
15-16,
hOV,197?
15.16,
Nov,1972
15-16,
hov,1972
15-16,
Nov,1972
15-16,
NOV,1972
15-16,
hOV,1972
G6-07>Oc
C,1972
c6-07.
cEc,1972
06-07,
CEC,1972
06-Q7,
cEc,1972
C6-07,0EC,1972
06-07,
06-07,
--—-
—.- . —..—.
GEc) 1972
cEc,1972
(EST)
TYPE
DATE
ELECTRON
TEMPERATuRE
ION TEMPERATURE
VERTICAL
IOh ORIFT
VERTICAL
ION CRIFT
cLECTROk
TE!4PERATuR[
IBN TEMPERATURE
vERTICAL
ION CRIFT
DENsITY
&LECTROh
TEMPERATURE
ION TEMPERATURE
vERTICAL
ION DRIFT
cLEt TROh TEMPERATURE
JON TEMPERATURE
VERTICAL
10N ORIFT
OENSITY
&LEc TROh TEFPERATURt
ION TEMPERATURE
VERTICAL
10b Uh’l FT
ELECTROh
TEt4PERATuRE
JON TKMFERATLRE
VERTICAL
ION ORIFT
OENSITY
&LECTROk
TEMPERATURE
ION TEMPE6ATuFiE
vERTICAL
Ioh
CRIFT
rLEc TRON TEHPLRATuRE
[ON TEMPERATURE
vERTICAL
ION DRIFT
—.
—..
—
RETIA5
0929
0929
0929
0929
0929
0929
1o11
KETf A5
RETIAS
RETIAS
RETIA5
RETIAS
L/LHF
L/bHF
L/bHF
L/utiF
L/bHF
L/LHF
L/LHF
RETIAS
RETIAS
RETIA3
WTIAS
RETIAS
RETIAS
RET IAS
RETIAS
RET IAS
RETIAS
1011
1o11
1o11
1011
1o11
lG1l
c819
c819
c819
c819
J819
0819
0819
08u9
0809
0809
0809
0809
0869
08D9
u928
0928
0528
0?28
0928
0928
J928
6929
0929
0929
0Y29
0929
0929
G929
RET IAS
I+ET IAS
RETIAS
RETIAS
L/bhF
L/LHF
L/LHF
L/LHF
L/b HF.
L/LklF
L/LHF
L/LHF
L/bHF
L/LHF
L/LHF
L/LHF
L/uHF
L/LHF
.—. .—.
-————
END
(EST)
1106
1106
1106
1106
1106
1106
1251
1251
1251
1251
1251
1251
1251
1043
1043
1G43
1C43
1043
1G43
1C43
1108
110s
1108
1108
1108
110$s
1108
1632
1632
1632
1632
1632
1632
1632
1603
16C3
1633
1603
1603
1603
1603
..-.
TEST VALUE
-.11237E
-,74026E
-026739E
-,11233E
-.73890E
-.26764E
.53781E
-.l1305E
-,74688E
-025270E
‘.11299E
-,7466f
E
-.252s6E
-053976E
-.78833E
-,6958?E
- ,253c5E
-,7?.830E
-.69261E
- .25295E
-,532o8E
-.1 OO54E
-,74985E
-.32869E
-,1 OO51E
-.74835E
-032397E
.49251E
-,77
L87E
-,62382E
-.25933E
,28773E
-.6241RE
‘.25965S
-,58992E
-,88118E
-,5+083E
‘.22533E
-.88085E
.5+324E
.3c370E
.
KDAT
203
303
1001
293
393
1091
04
03
33
04
03
03
ol
O+
03
03
04
03
03
01
03
iJ3
03
03
03
03
01
04
03
03
04
03
03
ol
03
C3
03
03
C3
03
“I
C3
03
101
203
303
1001
293
393
1091
1001
722560
722560
72256o
72256c
722560
722560
722562
72277>
72277C
72277o
72277c
72277o
72277c
72277c
7232C0
72320G
723200
723200
7232C0
723i?CC
723?!CC
72341G
72341C
723410
723410
293
393
1091
72341o
7.2341C
72341c
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
203
303
1001
293
393
1091
101
203
303
33
~3
C3
03
.
FIT NO.
72220C
72220G
72220G
72220C
722?OC
72220C
722500
72250C
7225CC
722500
72250G
722500
722500
.
. ..
..__”=..
,-
BIBLIOGRAPHIC QATA
SHEET
3. Recipient’s Accession No.
4. Title and Subtitle
5. Report Date
18 September 1978
Millstone Hill Thomson Scatter Results for 1972
6.
7. Author(s)
John V. Evans and John M. Holt
8. Performing Organization Rept.
No.
Technical Report 530
9. Performing Organization Name and Address
10. Project/Task/Work Unit No.
Lincoln Laboratory, M. I. T.
P.O. Box 73
Lexington, MA 02173
11. Contract/Grant NO.
ATM 75-22193
13. Type of Report & Period
Covered
12. Sponsoring Organization Name and Address
National Science Foundation
Atmospheric Science Section
Washington, DC 20550
Technical Report
14.
15. Supplementary Notes
16. Abstracts
During 1972, the vertically directed incoherent scatter radar at Millstone Hill (42.6”N, 71. SOW)
was employed to measure electron density, electron and ion temperatures, and vertical ion velocity
in the F-region over periods of 24 hours, one or two times per month. The observations spanned
the height interval 200 to 900 km, approximately, and achieved a time resolution of about 30 minutes.
This report presents the results of these measurements in a set of contour diagrams.
For a number of the days, the spectra of the signals gathered at altitudes between 450 and 1125 km
have been the subject of further analysis in an effort to determine the percentage of H+ ions present over
Millstone. The results suggest that Hf ions are escaping from the F-region to the magnetosphere at a
value close to the theoretical limiting flux during the daytime in all seasons. At night the flux becomes
downward commencing near midnight in winter, but may remain upward throughout the night in summer.
17. Key Words and Document Analysis.
170. Descriptors
Millstone radar
F-region
diurnal variations
electron density
ionospheric scatter
seasonal variations
temperature effects
magnetosphere
proton flux
17b. Identifiers/Open-Ended Terms
176. COSATI Field/Group
19.. Security Class (This
Report)
UNCLASSIFIED
18. Availability Statement
2 0 . Speacyity C’ ‘-’ .
FORM NTIS-35 (REV. 10-73)
ENDORSED BY ANSI AND UNESCO.
15 NCL
THIS FORM MAY BE RE
21. No. of Pages
132