Appendix A: DMSP Electron Data

O&C 31

a

a)

8S,

&
FEB 23

65]

ti)

14


rr rr a

6

| La a L Lia f Le \ La F
L L = | zz
| L ° L L ze *
zz
[ [ 2=z [ ze
[ [ ae [ Ze
L zz L 2 L 2 z2|
L z me [ wzez
[L o # [ ze [ =|
[L L zz" f L 2
s ° a L oF L z2 =F L =
z [ He [ 2 bee =| Zz
3 a L z L 222 L 2
é L mee Ct “Ef = 2#"
A L oa L zz ze L
z lo» [ % L a? | =
E-) psa L ° L L =
3 in gL | z = L 2 =|
3 BA L 9 L zee 7 | 2 |
< Ooh wo L | 2 eA L zz ym
o gan L o + a2) | ee
Le = = ° iF L Zz
z ov L = | L z z
wo L a L L 2 72%
D ih L Zn wl L L z
ra) | “ | 2 L 2a oe
m a L L Be
og Pay ot eg po oo oo se
Oo wn oO ~ oOo wn DD oo wo wo ~ oO

~ oa S
AUG 31 7S SEP 27 75 oct 24 75 NOV 20 75



Appendix B: DMSP Optical Data

fl 4 fl 1 poy \ 4 1 \
@anp L Poly Fy [
Gay © | ® typ
o L Rp, o ABE?
Xp, L ok as
Se L aD Hon qo zo
Pap, | ny CPly [ [ 2A ol
AB les [ ® vw | ney L | ne
PB wy L @hy, | L &
DAH On ez
PO L Sox L L
8 1 L L wo
AS? L L B [
wo
4 wo vol L L
wn Mm w L L L.
PHP L L L 2y
wn L L wo L wo
o 2 vol L Boi - oF
2) wn bes [ L Ly L hy
L Pp L ah L
on L eo 8 L a) L
L,
n> b wn an L L
ole L wo [ L pra
L bn L OR 1 ress
op L B® be L ° Oo, L oR 1%?
2 wv L Ly L nn Mh on L ° DP
ee
2) em | Berto | ep wl &
wo
on | HP | o pee |
Bolo 7h 2, ole, a
@ ¢ “g8 "¢ "8 "ge "8 "6 "BB eB
JUN 2574 JUL 22 74 AUG 18 74 SEP 14 74

31


Lu 1 _L ae 4 L _L " 4. ao LL J. 1 —t L L 4 L a —L
zz L WB ben | Pao | etn |
2 L L BR, P| A Br) L
L ope L zh oe O°” Ba zl L
z
z L no" L Pes, L 0 on He L
z L ow o | rn o L Ath L
z bh w
= + op L “ee L ” L
= ow b L
2 L L
z o vin L L
Zz 7 r wn
be we =
L - tf
£ L > | oF op L L
a L L ” L L
& = “261 L On Zz L
2 = L L
cc} 27 L L Zin L 8 On L
& | L Cn Be L ” L
a L L ne L ” Mn n L
[--} L L Bar L OG, L
%
: [ [ ie [ oof
Hl > Pn
a | 2+ pk L
< [ z2zt L 0 DP Bh L L
Zz L L | © L L
- r 2 [ vn Sb [ o [
z L - L i a | L
z x OFZ op i. Me Tn L
z r z r o
z] | zz L twP zap L on a L
z L Ze [ woe L o L
a2 22 iz ® the non [
L L L
2 age » no
r r ae
g "eg "ed "#8 g €  ¢@ 'g28 '¢ "8 ag g 8 8
FEB 21 77 MAR 20 77 APR 16 77 way 13°77

40


AKASOFU, S.-I.

BELL, B. and
J. NOCI

DANDEKAR, B.S.

EVANS, J.E.,
L.L. NEWKIRK and
B.M. MC CORMAC

FELDSTEIN, Y.I. and
G.V. STARKOV

NEUPERT, W.M. and
V. PIZZ0

NOLTE, J.T.,
A.S. KRIEGER,

1974

1976

1979

1969

1967

1974

1976

A.F. TIMOTHY, J.S. VATANA,

and M.V. ZOMBECK
SHEELEY, JR., N.R.
J.W. HARVEY and
and W.C. FELDMAN

SHEELEY, JR., N.R.

1976

1978

SHEELEY, JR., N.R. and 1980

R.A, HOWARD

References

"A Study of Auroral Displays Photographed From the DMSP-2 Satellite and

From the Alaska Meridian Chain of Stations," Space Sci. Rev., 16, 617

"Intensity of the FexV Emission Line Corona, the Level of Geomagnetic
Activity, and the Velocity of the Solar Wind," J. Geophys. Res., 81,
4508-4516. ~

"Study of the Equatorial Edge of the Auroral Oval from Satellite
Observations" (Report AFGL-TR-79-0010, Air Force Geophysics
Laboratory, Hanscom AFB, Massachusetts 01731).

“North Polar, South Polar, World Maps and Tables of Invariant
Magnetic Coordinates for Six Altitudes: 0, 100, 300, 600, 1000,
and 3000 km," (Report No. DASA 2347, Lockheed Research
Laboratory, Palo Alto, California).

“pynamics of Auroral Belt and Polar Geomagnetic Disturbances,"
Planet. Space Sci., 15, 209-229.

"Solar Coronal Holes as Sources of Recurrent Geomagnetic
Disturbances," J. Geophys. Res. 79, 3701-3709.

-725.

“An Atlas of Coronal Hole Boundary Positions May 28 to November 21, 1973,"

Solar Phys. 46, 291-301.

“Coronal Holes, Solar Wind Streams, and Recurrent Geomagnetic
Disturbances: 1973-1976," Solar Phys., 49, 271-278.

"The Equatorward Extent of Auroral Activity During 1973-1974,"
Phys., 58, 405-422.

Solar Phys. (in press)

Solar



a nl a 1 a a re !
Prnh L Prox, L ot L
Pan PO L ® ts L Oo ox L
o t PR, L er gen L
Po + om L earl L
Ft [ ow ong | L
PF asin | Pak L L
OB boen L PB | Hey L [
# Po oy L ope | }
é Ww Bun L 20 byprn | L
z B L L L
5 oe? L L B L
o
8 ool L L
£ Pr L L L
z o [ L ° [
ee o Oe r a r
= ~ L L in |
a
iS) F F ° F
z a «4 L o 9 L en L
z [ oe | oe L
& ao] oa L ” L BR L
g L ne OR |
° ep L ® wy L ° YBa | L
2 aby [ L, [ An oy |
ow | Brey | Po ool
Pm wm | FB | _ cn
Bolo ? Reh 0 POD boy
rr er er ee ee er a ae ge

e
JUN 25° 74 JUL 2274 AUG 18 74 SEP 14 74

50


Appendix C: DMSP Electron and Optical Data

NWN

t—F
N

JAN

WY 74

48


Appendix C: DMSP Electron and Optical Data

RB
5s §

BON

a

AUG 31

83,

x
7 T
ec

SEP 27 75

65!

ocT 24

18

5a


AON

SL

930

SL

6e 330

SL

LL Se NUP

Appendix C: DMSP Electron and Optical Data



udb

el 61

ADH

el gt

el NAL

€L

nr

€L

Appendix C: DMSP Electron and Optical Data

46



8S. Appendix A: DMSP Electron Data

93.
Bo,
Sa
Bow wy
285
Be
eed
ERR
ioe
ae

uBH

OL

Yd

9L Of Hd
R
D»D
aS
in
x
a
op
Fle om
? owe,
Se
pee
C~
—
Pos,
Bw
ws
Bp



Appendix B: DMSP Optical Data

a 1 fr a ee 1
222 2a
4z ae az [ mw Azeem
zz eee zee
ae aw B=
zee 2
zu L |
i 3
= zt a
2zat L 2 ate
a zazz Be
2 [ 2
Be L 2
ze [ Be
| =
zz [ ae
ae 2er
+ sf
z L z zeae =
z [ 2 22ie
ae L =
2 ke | zz Zab
Zoe BE L z
zm = L we ®
ame L =z
2 ee L BA
=z FT 2
gd ' ov * UY ee, r
Do ~ wo Ww oa ~ wo
DEC 17 75 JAN 13° 76

boa \ 14 \
2 L L
z
z L ze
= L L
z=
L L
Zz = L =z) L
2 Bz L z L
2m
L z Lo
zz = zzz /
a= k z L
z I L
2 Be [ 2 L
2ue L z L
= az
z= L = Bee L
a Pee a
zz SF | = | |
zoe L dq i
Bz 2s
2" [ ze [
22 = L
2E* [ we L
mz 4 zzz
zeae L ze L
ze L z 22|= L
ze L 2 az [
72 [ 3 [
z q Zz
—# r op
é'6 gp ¢8 "8 "8 "8
FEB 9 76 MAR 7 (76

36


CONTENTS

Introduction . 6 6 ee eee ee ee ee ee ee ee ee

Data Reduction.Techniquese . +...

Temporal Plots of Equatorwardmost Invariant Latitude ....

Daily Index of Equatorwardmost Auroral Latitude... 2...

Acknowledgments. se se eee eee eee

References . se ee ee ee ee ene

Table 1. Observations with A<45°. 2. we

Table 2. Observations with 45°<a<50°.

Table 3. Observations with 50°<A<55°

Appendix A:
Appendix B:
Appendix C:

DMSP Electron Data... .
DMSP Optical Data... .

OMSP Electron and Optical

Tables

Appendixes.

Data, wee ee eee

Page

10

43



Appendix B: DMSP Optical Data

uf
i

W411 1 L \ \ rn L a \
z aoe z=
am r ae 2K 2 r 2 wee eo

2 2 zzz
z = [ 2 Zz
=z 7 r [ ze zm
2 i. ae [ 2 ze
z ze ae zl =
r zz i. = 224 a
y = r * zit 2
z ez Ezz [ z= 23
z F z2F es oe.
2 222 [ a FF | zz 2
zZ L zeae L z 24z
2 2@z | Beez [| ze
2 2a ar | 2 2 22
2 22 [ Ce ae 222ze 7
zz a L ee Lak =
BJ [ er of ghz
ae F [ aa [ 2
#L [ we 2
z & [ ae [ Zz
zezz ie L 2 =z [ =
“i [ aT =e/ 2
a:
Zee i Pe [ [
z z L z L 2
2eel= Boz zy
zezf Zz i. z
“¢ "8 "8g g gé ° 8 8. "gg "g " 8
NOV 21 73 DEC 18 73 JAN 1474 FEB 10 74

29


SL ¢@@ YbW

udb

SL 81

ABW

St SI

Tt NAP

SL

Appendix A: DMSP Electron Data

B

wen ger

B

8,
8
784
lye p fl
sg Be
58, T T T T
83,

75)

+

65]

55.

8

754

55.

85,

T



Appendix A: DMSP Electron Data

9 ta,

83,

“fen f
a ao

JAN 25 77

S&L

APR 16 77

2


Appendix A: DMSP Electron Data

wl
%

Peed heal T
i o
TCT 2b 75

S

NOV 20 75

uw
©

wo

i

OEC

rr)

oO
17, (78

JAN 13 76

v7


Appendix B: DMSP Optical Data

111+

T

Qn
? Pago
PP orp,

pel”

5S.

foot gt gg
i 6
MAY 23° 74

rw
i)

30


Appendix A: DMSP Electron Data

12

a oe L [a or n a L a
a G a =
0 F cy r r
a x F «
L ion L L
0 ERE og L L L
fe
© @|c L cS L o L
ae fon
L om L L
gq «
om L DT eh L L
x L o L L
Mee L ar L L
a x a qd
wet L L L
ee
coc coal | o @ L r
fond
ang L oa L L
2° € °
i. oe . L
not & jc
o\o r oo GO r r
ce
BD co L ame | oP L
op |~ a o Ey L a
oof Joe L ay L =
a € o «
ger
c
oh L a [ fos |
oO c
=arS L a € L L
et L a) L L
« 8 L awe de L aa L
L gq b on ob
oa
Fe Ts Ts, TT; : c)
oO ~ oO ite) o ~~ wo wo o ~ wo wo ao ~

FEB 10 74 MAR S74 APR STU MAY



udd

SL

QL le ABW SL OF Hdd

92 €e@ NAF

Appendix C: DMSP Electron and Optical Data

T



Table 2. Observations with 45°< a <50°

Date Time Cat Tong A Date Time Lat Long A

72 916 0919 -65.3 306 49.3 75 2 14 0731 53.5 98 48.6
72 10 14 = 1056 43.2 193 47.2 75 215 0529 50.0 71 45.1
72:10 14 1242 51.9 164 46.8 75 2 15 0712 «52.2 95 47.4
721018 1144 -37.4 171 47.4 75 2 16 0512 53.1 64 47.8
72 10 28° 0846 54.3 145 48.9 75 2 16 0654 «51.5 90 46.8
72 1119 1408 $1.3 146 46.0 78 3 1 0615 52.2 80 47.3
72:11 29 (O15) 53.9 122 48.8 75 3 2 0556 451.3 75 46.6
72 11 30 1453 54.5 162 49.4 75 3 3 0537 54.1 69 48.8
72:11 30 1634 54.0 137 48.7 75 3 3 0718 «454.3 93 49.3
7212 5 1401 49.9 86 45.3 75 3 16 0458 «453.3 60 48.0
73-3 8 1635 53.0 105 48.1 75 317 0440 453.0 55 47.7
73,321 1648 49.8 104 45.3 75 317 0622 50.8 82 46.0
73 429 = 1738 50.0 91 45.4 75 4 30 0936 ~-59.0 243 49.4
73 617 0854 53.2 223, 48.3 75 7 30 0358 -51.5 214 49.1
73 618 1033 -63.2 296 47.3 75 8 28 1126 -53.6 236 45.7
73 6 29° 0737 50.6 156 45.3 75 8 30 1049 51.5 134 46.3 E
73° 6 29° «(1618 53.5 110 48.6 75 9 9 1100 -49.0 11 49.1 €
73°7 12 (1713 53.0 91 48.1 75 10 14 1757, 51.1 29 46.3 E
73°7 3 = 0835 64.7 -54 48.7 75 12 10 1728 (52.4 36 47.3 E
73 8 23 0645 -61.4 343 48.7 E 76 1 9 1914 53.0 11 49.8
73,9 21 = 1433 -51.1 226 45.8 76 19 1948 -64.3 332 49.5 E
74 10 12 0725 52.7 99 47.9 719 2130 -65.8 305 49.8 E
74:11:10 0131 52.8 85 47.9 76 117 1054 53.9 112 48.9 E
74:11 10 0507 52.3 65 47.1 76 3 26 1618 55.4 57 50.0 E
74 11 10 0648 51.7 91 47.0 76 4 5 1922 -59.9 343 47.5 E
74 11 11 0448 54.4 59 49.0 76 4 5 2105 -65.8 312 49.9 E
74 11 11 0630 52.4 86 47.5 76 4 6 1906 -59.7 347 48.5 E
74 11 20 0039 51.9 72 46.8 76 4 7 1906 -58.6 347 47.9 E
74:11 22 (0147 53.8 89 48.8 76 4 8 2019 -65.2 324 49.7 E
74:12 10 0416 54.7 51 49.3 76 4 9 1818 -54.7 1 49.6 E
74:12:10 0559 50.7 78 45.9 76 418 1925 -63.2 340 49.4 E
74:12 11 (0549 50.4 74 45.5 76 4 19 1908 -60.6 346 48.9 £
74:12 12 ©0522 $1.2 69 46.1 76 4 20 1852 -59.3 350 49.4 E
75 1 9 0508 52.0 64 46.8 76 4 22 1820 -54.4 1 49.4 E
75 1 9 0650 52.8 85 47.9 767 9 0424 -58.4 237 49.9 E
75 110 0631 53.8 84 48.8 77 2:13 0340 -57.1 248 46.6 €
75 2 2 0017 $1.1 78 46.2 E 77 2 2 0934 «54.1 134 48.8 E



Appendix B: DMSP Optical Data

61 ddd

el

ABW

el gt

Nar

a

el



UAG-26

UAG-27

UAG-28

UAG-29

UAG-30

UAG-31

VAG-32

UAG-33

UAG-34

UAG-35

UAG-36

UAG-37

UAG-38

VAG-39

UAG-40

UAG-41.

UAG-42

VAG-43

UAG-44

UAG-45,

UAG-46

UAG-47

UAG-48A

UAG-49

UAG-50

UAG-51.

“Data Compilation for the Magnetospherically Quiet Periods February 19-23 and November 29 - December 3,
1970," compiled by Helen E. Coffey and J. Virginia Lincoln, World Data Center A for Solar-Terrestrial
Physics, NOAA, Boulder, CO, May 1973, 129 pp, $0.70.

“High Speed Streams in the Solar Wind," by D.S. Intriligator, University of Southern California, Los Angeles,
CA, June 1973, 16 pp, $0.15.

"Collected Data Reports on August 1972 Solar-Terrestrial Events,” Parts 1, 2 and 3, edited by Helen E.
Coffey, World Data Center A for Solar-Terrestrial Physics, NOAA, Boulder, CO, July 1973, 932 pp, $4.50.

“Auroral Electrojet Magnetic Activity Indices AE(11) for 1968," by Joe Haskell Allen, Carl C. Abston and
Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, October 1973, 148 pp,
$0.75.

"Catalogue of Data on Solar-Terrestrial Physics," prepared by NOAA Environmental Data Service, Boulder, CO,
October 1973, $1.50. Supersedes UAG-11, 15, and 20 catalogs.

“Auroral Electrojet Magnetic Activity Indices AE(11) for 1969," by Joe Haskell Allen, Carl C. Abston and
Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, February 1974, 142 pp,
$0.75.

"synoptic Radio Maps of the Sun at 3.3 mm for the Years 1967-1969," by Earle 8. Mayfield, Kennon P. White
ITT, and Fred I. Shimabukuro, Aerospace Corp., £1 Segunda, CA, April 1974, 26 pp, $0.35.

"Auroral Electrojet Magnetic Activity Indices AE(10) for 1967," by Joe Haskell Allen, Carl C. Abston and
Leslie, Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, May 1974, 142 pp,
$0.75.

“Absorption Data for the IGY/IGC and IQSY," compiled and edited by A.H. Shapley, National Geophysical and
Solar-Terrestrial Data Center, Boulder, CO; W.R. Piggott, Appleton Laboratory, Slough, UK; and K. Rawer,
Arbeitsgruppe fur Physikalische Neltraumforschung, Freiburg, GFR, June 1974, 381 pp, $2.00.

“Catalogue of Digital Geomagnetic Variation Data at World Data Center A for Solar-Terrestrial Physics,"
prepared by NOAA Environmental Data Service, Boulder, CO, July 1974, 20 pp, $0.20.

“an Atlas of Extreme Ultraviolet Flashes of Solar Flares Observed via Sudden Frequency Deviations During the
ATH-SKYLAB Missions," by R.F. Donnelly and E.L. Berger, NOAA Space Environment Laboratory; Lt. J.D. Busman,
NOAA Commissioned Corps; 8. Henson, NASA Marshall Space Flight Center; T.8. Jones, University of Leicester,
UK; G.N. Lerfald, NOAA Wave Propagation Laboratory; K. Najita, University of Hawaii; W.M. Retal lack, NOAR
Space Environment Laboratory and W.J. Wagner, Sacramento Peak Observatory, October 1974, 95 pp, $0.55.

“Auroral Electrojet Magnetic Activity Indices AE(10) for 1966," by Joe Haskell Allen, Carl C. Abston and
Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, Decenber 1974, 142 pp,
$0.75.

“Waster Station List for Solar-Terrestrial Physics Data at WOC-A for Solar-Terrestrial Physics,” by Rel.
Buhnann, World Data Center A for Solar-Terrestrial Physics, Boulder, CO; Juan D. Roederer, University of
Denver, Denver, CO; and M.A. Shea and D.F. Smart, Air Force Cambridge Research Laboratories, Hanscom AFB, MA,
December 1974, 110 pp, $1.60.

“Auroral Electrojet Magnetic Activity Indices AE(11) for 1971," by Joe Haskell Allen, Carl W. Abston and
tes}ie 0. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, C0, February 1975, 144 pp,
2.05.

“H-Alpha Synoptic Charts of Solar Activity for the Period of Skylab Observations, May 1973 - March 1974," by
Patrick S. McIntosh, NOAA Space Environment Laboratory, Boulder, CO, February 1975, 32 pp, $0.56.

“H-Alpha Synoptic Charts of Solar Activity During the First Year of Solar Cycle 20 October 1964 - August
1965," by Patrick S. McIntosh, NOAA Space Environment Laboratory, Boulder, CO and Jerome T. Nolte, Anerican
Science and Engineering, Inc., Cambridge, MA, March 1975, 25 pp, $0.48.

“Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-80 MHz, 10 December 1971 through 21 March
1975," by James W. Warwick, George A. Dulk and Anthony C. Riddle, University of Colorado, Boulder, CO, April
1975, 49 pp, $1.15.

"Catalog of Observation Times of Ground-Based Skylab-Coordinated Solar Observing Programs," compiled by Helen
E. Coffey, World Data Center A for Solar-Terrestrial Physics, NOAA, Boulder, CO, May 1975, 159 pp, $3.00.

“synoptic Maps of Solar 9.1 cm Microwave Emission from June 1962 to August 1973," by Werner Graf and Ronald
N. Bracewell, Stanford University, Stanford, CA, May 1975, 183 pp, $2.55.

"Auroral Electrojet Magnetic Activity Indices AE(11) for 1972," by Joe Haskell Allen, Carl C. Abston and
Leslie D, Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, May 1975, 144 pp,
$2.10 (microfiche only).

"Interplanetary Magnetic Field Data 1963-1964," by Joseph H. King, National Space Science Data Center, NASA
Goddard Space Flight Center, Greenbelt, M0, June 1975, 382 pp, $1.95.

“Auroral Electrojet Magnetic Activity Indices AE(11) for 1973," by Joe Haskell Allen, Carl C. Abston and
Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, June 1975, 144 pp,
$2.10 (microfiche only).

“synoptic Observations of the Solar Corona during Carrington Rotations 1580-1596 (11 October 1971 - 15
January 1973)," [Reissue of UAG-48 with quality images], by R.A. Howard, M.J. Koomen, D.J. Michels, R.
Tousey, C.R. Detwiler, D.E. Roberts, R.T. Seal, and J.0. Whitney, U.S. Naval Research Laboratory, Washington,
DC, and R.T. Hansen and S.F. Hansen, C.J. Garcia and E. Yasukawa, High Altitude Observatory, NCAR, Boulder,
CO, February 1976, 200 pp, $4.27.

“Catalog of Standard Geomagnetic Variation Data," prepared by NOAA Environmental Data Service, Boulder, C0,
August 1975, 125 pp, $1.85.

“High-Latitude Supplement to the URSI Handbook on Ionogram Interpretation and Rediction," edited by WR.
Piggott, British Antarctic Survey, c/o Appleton Laboratory, Slough, UK, October 1975, 294 pp, $4.00.

“synoptic Maps of Solar Coronal Hole Boundaries Derived from He II 304A Spectroheliograms from the Manned
Skylab Missions," by J.D. Bohlin and D.M. Rubenstein, U.S. Naval Research Laboratory, Washington, OC,
November 1975, 30 pp, $0.54.



UAG-76 “Auroral Electrojet Magnetic Activity Indices AE(12) for July-December 1975," by
c t 2" by J.H. Allen, C.C. Abston, J.E.
and J.A, McKinnon, National Geophysical and Solar-Terrestrial Data Center, NOAA, Boulder, CO, fngust 1900, 320 pp aed.

UAG-77 “Synoptic Solar Magnetic Field Maps for the Interval including Carrington Rotations 1601-1680, May §, 1973 -
April 26, 1979," by J. Harvey, 8. Gillespie, P. Miedaner, and C. Slaughter, Kitt Peak National Observatory,

Tucson, AZ, August 1980, 70 pp, $2.50.



Appendix B: DMSP Optical Data

2a

s

mn

= Br
a

rat

55.

AUG 19 72

65.


OPTICAL AND ELECTRON MEASUREMENTS OF THE EQUATORIAL AURORAL
BOUNDARIES DURING 1972-1977

N. R. Sheeley, Jr. and R. A. Howard
E. 0. Hulburt Center for Space Research
U.S. Naval Research Laboratory
Washington, D.C. 20375

and

B. S. Dandekar
Air Force Geophysics Laboratory
Hanscom AFB, Mass. 01731

ABSTRACT

The equatorial latitude of auroral activity has been derived from both electron and
optical observations with the DMSP satellites. Essentially all of these observations
have been used to produce a nearly continuous plot of invariant geomagnetic latitude
versus time during the 5-year interval June 1972 - September 1977. This plot has two
main characteristics: (1) a diurnal variation of approximately +5° which is somehow
associated with the precession of the Earth's magnetic dipole axis about the Earth's
rotation axis and (2) an irregular variation of roughly 5-10° for intervals of one to
several days associated with the occurrence of solar flares and coronal holes. With
the help of a condensed, Bartels-type display of these measurements, we conclude that
(1) modest auroral expansions (to A~ 60°) occur during the main body of high-speed
streams from coronal holes and (2) great expansions (to A < 55°) occur only during
intervals of intense interplanetary magnetic fields, such as may occur at the leading
edge of a high-speed stream or at a flare-produced interplanetary shock.

Introduction

Using solar, interplanetary, and geomagnetic observations during the declining phase (1972-1976) of sunspot
cycle 20, several workers found a high degree of correlation between the occurrence of coronal holes, solar wind
high-speed streams, and recurrent geomagnetic disturbances [cf. Bell and Noci, 1976; Neupert and Pizzo, 1974;
Nolte et al, 1976; Sheeley et al, 1976]. Later, Sheeley [1978] used auroral observations obtained in the U.S. Air
Force Défense Meteorological Satellite Program (DMSP) during 1973-1974 to compare the variations of auroral
latitude with the occurrences of coronal holes and solar flares during the Skylab era. The transits of Tow-
latitude coronal holes across the solar disk were accompanied by expansions of the Earth's auroral ovals to
invariant latitudes that were often less than 60°. Comparable, flare-induced expansions were rare during the
Skylab era, but a few major events with expansions to 53° latitude did occur in 1972.

Subsequently, in 1978 we decided to analyze all of the DMSP auroral observations that were then available.
These data consisted of both electron and optical observations for both Northern and Southern Hemispheres of the
Earth during the interval June 1972-September 1977. The measurements of equatorwardmost auroral positions were
transformed from geographic coordinates to invariant geomagnetic latitude and plotted versus time in 27-day
segments for comparison with solar phenomena.

The optical and electron observations are plotted both separately and together. Sheeley and Howard [1980]
were interested primarily in the correlation of oval size with the occurrence of solar phenomena so they used the
combined data set to increase their statistical sample. Dandekar [1979] has analyzed these DMSP optical
observations for the dependence of the equatorial edge of the auroral oval on the magnetic activity indices Kp and
Q. However, to benefit researchers with other interests, we have included large-scale plots of both the separated
and the combined data in this report.

Data Reduction Techniques

. As described elsewhere [Sheeley, 1978; Sheeley and Howard, 1980], the measurements of equatorwardmost auroral
latitude were derived from the Air Force DMSP auroral analysis records. These records contained the geographic
coordinates of the equatorial boundary of the auroral activity as a function of time on an orbit-by-orbit time
scale. We simply transformed from geographic coordinates to invariant geomagnetic coordinates using the published
maps of Evans et al. [1969] for the 100-km level. In practice, we approximated these maps by a closed-form
algebraic expression which gave invariant geomagnetic latitude with an accuracy of +1°. Dandekar [1979] has
discussed the nature and limitations of these DMSP optical data.

We obtained the auroral analysis records in several sections. The largest section was transformed to
magnetic tape at the Air Force Geophysical Laboratory (AFGL). However, this section did not include a 6-month
interval during the first half of 1973 as well as several other smaller intervals during the subsequent four
years. We obtained the 6-month section in tabular form on microfilms made available by the USAF Air Weather





Appendix A: DMSP Electron Data

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Table 1. Observations with a<45°

Date Time Lat long A

72 8 16 1644 =53.1 295 37.3
7211 1 = 1802 44,7 14 40.9
7211 4 1649 41.6 67 (37.1
73-2 9 1612 45.3 76 40.8
73° 3:12 1537 -50.7 240 42.1
73° 413 0428 -58.0 297) 42.1
73 4 30 = 1536 52.5 238 44.2
73 4 3001718 -51.5 263 38.7
73,5 1 1822 -56.6 304 = 40.6
73 5 6 1915 -58.3 303 42.3
73518 0034 -50.8 284 35.7
73:5 18 2224 23.0 79° 20.4
73° 5 23 0805 -55.0 250 44,2
73° 5 27 2202 59.9 326 44.6
73,612 1009 -52.8 242 43.7
73 6 20 0323 -58.1 294 42.3
73 8 1 1648 ~52.5 250 «41.8
73825 1505 45.7 63 40.8 E
74 9 20 2002 -14.6 342 «16.4 E
74 10 26 0624 49.3 86 44.7
75 616 0925 ~49.7 226 44.4
75 7 8 1006 -52.3 238 44.2
75 812 1001 -59.0 296 43.1
76 5 7 0346 71.4 245 6.3
76 515 0140 58.2 278 «643.5 E
76 7 7 1517 2.0 88 2.0 E
76 10 17 = 0832 46.5 191 43.5
7611 1 0110 46.4 82 42.0 E
77-912 ~=«0552 -51.0 274 = 36.8
77 9 23 1700 43.2 3538.0 E
77.9 23 2356 42.5 203. 41.5 E



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WORLD DATA CENTER A

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REPORT UAG-78

THE EQUATORIAL LATITUDE
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AURORAL ACTIVITY DURING 1972-1977

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A Daily Index of Equatorwardmost Auroral Latitude

Sheeley and Howard [1980] summarized all of the A -measurements on a daily basis to facilitate their
comparison with solar phenomena such as coronal holes and solar flares. For completeness, we have reproduced
their summary here. A "J-index" of daily minimum A was constructed as follows: First, for each day, the minimum
latitude for the electron data and the minimum latitude for the optical data were identified. Then, to reduce the
possible influence of sporadic data points, these two values were averaged. When only one kind of data was
available the minimum latitude for that kind was used. Finally, an index on a scale of 0 to 7 was assigned
depending on the location of this latitude, < A min>, within one of the following 2,.5°-latitude ranges:

<A min> J
72.5-75.0 0
70.0-72.5 1
67.5-70.0 2
65.0-67.5 3
62,5-65.0 4
60.0-62.5 5
57.5-60.0 6
§5.0-57.5 7

Also, J=7 was used whenever < A min> was less than 55°. (This "saturation" of the J-index was determined after
< A min> had been calculated from individual latitudes, one or both of which may have been less than 55°.)

The J-index is compared with the C9 index of geomagnetic activity in a 27-day Bartels-type format during the
interval June 1972-September 1977. In the J-index format, blank spaces without entries correspond to days for
which auroral latitude measurements were not available. The agreement is only fair considering the fact that the
electric currents in the auroral ovals are supposed to be the source of the fluctuations of the geomagnetic field
and vice versa [cf. Banks and Doupnik, 1975]. Some sporadic discrepancies were caused by errors in the
measurement of auroral latitudes and their transposition from the A-plots to the J-index. See Fig. 1. Other dis-
crepancies may have resulted from the paucity of observations during specific time intervals.

On the other hand, each display shows the same long-lived recurrence patterns that are associated with
coronal holes and high-speed solar wind streams [cf. Sheeley and Harvey, 1980]. Typically, C9 indices in the
range 5-7 correspond to J indices that are also in the range 5-7 (A in the range 55.0° - 62.5°). This relation
seems to have been characteristic of the auroral expansions that were associated with high-speed streams from
coronal holes during 1973-1977. As Sheeley and Howard [1980] have discussed in detail, auroral expansions below
55° occurred only during intervals of intense interplanetary magnetic field strength such as were present
occasionally at the leading edge of a high-speed stream or at a flare-produced interplanetary shock. The reader
is referred to the papers by Sheeley [1978] and Sheeley and Howard [1980] for a more detailed discussion of these
observations and their relation to solar phenomena.

Acknowledgments

The DMSP auroral imagery and analysis records were made available by the USAF Air Weather Service through the
National Geophysical and Solar-Terrestrial Data Center, NOAA, Boulder, Colorado. Also we thank the Space
Environment Support Branch of the Air Force Global Weather Central, Offutt AFB, Nebraska for providing the DMSP
satellite data. We are also grateful to H. W. Kroehl (NOAA) and C. -I.Meng (JHU/APL) for useful discussions and
to D. J. Michels (NRL) for loaning us copies of the 1973-1974 auroral observations that he had purchased from
NOAA. Financial support at NRL was obtained from NASA DPR W-14, 429, Finally, we are grateful to the staff of
the World Data Center A for Solar-Terrestrial Physics for both encouraging this work and for publishing this final
report.



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25


UAG Series of Reports

Between 6 and 12 UAG Reports are published at irregular intervals each year. Subscriptions may be ordered through the
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UAG-2 "A Reevaluation of Solar Flares, 1964-1966," by Helen W. Dodson and E. Ruth Hedeman, McMath-Hulbert
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UAG-3 “Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-41 MHz, 6 July 1966 through 8 Septenber
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UAG-23 "“U.R.S.1« Handbook of Ionogram Interpretation and Reduction," Second Edition, November 1972, edited by W.R.
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Service through the NOAA National Geophysical and Solar-Terrestrial Data Center (NGSDC). Most of the smaller
sections were also supplied in tabular form by the NOAA NGSDC courtesy of H. W. Kroehl. These tabular data were
punched onto cards and transferred to magnetic tape for processing with the large section of data from AFGL.

Despite our attempts to be complete, several sections of data are still missing. Some sections seem to have
been lost or loaned to individual users and long forgotten. (The January 1973 optical data fall in this category
because published images during this interval can be found in the literature [cf. Akasofu, 1974]). Other sections
include times when electron observations or optical observations (or both) were not obtained. Of course, during
each solstice optical data were not obtained in the Earth's summer hemisphere.

Temporal Plots of Equatorwardmost Invariant Latitude

This part of the report contains plots of the equatorwardmost latitude of auroral activity on an orbit-by-
orbit time scale. The optical measurements begin in June 1972 and extend (with some interruptions) through
September 1977. The electron measurements begin in August 1973 and also extend through September 1977. Invariant
geomagnetic latitude, A, is plotted versus time in 27-day segments for comparison with solar phenomena. Optical
data in the Northern and Southern Hemisphere are indicated by the letters N and S, respectively, in Appendix
B. Electron data are indicated by the letters A (north) and B (south) in Appendix A. In the combined data, the
points often overlap so much that the letters cannot be distinguished (Appendix C). Sheeley and Howard [1980]
regarded this overlap as evidence that either kind of auroral data can be used for comparison with solar
phenomena.

Our plotting technique suffers from two drawbacks. The first drawback is a systematic error that was not
discovered until all the data had been plotted. Namely, each point was plotted approximately 1.4° higher in
jatitude than it should have been. Consequently, this relatively small correction of 1.4° must be subtracted from
each plotted A-value in order to obtain the correct invariant geomagnetic latitude (which itself has been derived
with an accuracy of 41°.)

The second drawback jis that the plot "saturates" for values of A less than 55°. Coupled with the first
drawback, this means that whenever we obtained a value of A that was less than 55°, we arbitrarily plotted that
point at the latitude of 56.4°. Thus, in the September 14, 1974 Bartels rotation (electron data) some of the
points at 56.4° probably had values less than 55°. For example, the "saturated" points on September 15-16 may
correspond to relatively great expansions of the auroral ovals. However, the other "saturated" points in this
Bartels rotation probably indicate measurement errors because each one is widely separated from the remaining
points on the same day. (We estimate that roughly 1-2% of all the measurements are incorrect due to a combination
of human errors in the various stages of observation and reduction of the data. Based on 30,000 total data
points, this amounts to 300-600 total errors or roughly 5-10 errors per Bartels rotation.)

When such "saturated" points are real, they are of particular interest because they are often associated with
exceptional interplanetary conditions. Consequently, for completeness we have tabulated all of these “saturated"
points despite the high probability that many of them are measurement errors. They are summarized in Tables 1, 2,
and 3 according to whether the calculated value of A was in the range 0-45°, 45-50°, or 50-55°, respectively. In
these tables, the symbol E refers to electron observations.

In their highly compressed 27-day format, the A-plots seem rather noisy. Short-term variations of
approximately +5° are always superimposed on the long-term variations of latitude regardless of the season of the
year or the interplanetary conditions. In fact, during each 27-day interval the plot appears as a 10° -wide band
that weaves back and forth between the 55° and 75° latitude extremes.

Whereas the longer-term meandering undoubtedly indicates real expansions and contractions of the sizes of the
auroral ovals in response to changing interplanetary conditions, the amplitude of the diurnal variation is much
too large to be real. Indeed, a 10° increase in the radius of an oval would be comparable to the expansion that
is typically associated with a large magnetic storm [cf. Feldstein, and Starkov, 1967]. Thus, Sheeley and Howard
[1980] assumed that the diurnal variation is mainly an “eccentricity" effect caused by the misalignment of the
Earth's magnetic dipole and rotation axes, and by the consequent sampling of different parts of the ovals at
different local times.

It is instructive to consider the diurnal variation briefly despite its probable sampling origin. The
variation is particularly clear in the separate plots of electron and optical data. In the electron observations
(both hemispheres included, but not distinguished), the phase of this variation seems to remain essentially
unchanged throughout the interval August 1973-September 1977 independent of the season. On each day, A tends to
reach its maximum value at 0700 + 0200 UT and its minimum value at 1900 + 0200 UT. The optical observations show
essentially this same phase during November-February when Northern Hemisphere data are available. Figure 6 of the
paper by Sheeley [1978] illustrates this variation on an expanded time scale.

The optical observations show a different behavior during May-August when Southern Hemisphere data are
available. In these measurements, there is a tendency for A to reach its maximum value a few hours after noon and
its minimum value a few hours after midnight universal time. However, this tendency is present only about half of
the time. On the remaining days, the points are either widely scattered or distributed nearly vertically in
the A-plots.



Appendix A: DMSP Electron Data

ao
oma TE
er
afta, F
€ Ss
co L
Se L L
2 oS [ © [
rar
os L .
oc L L
one L © L
€ Ea
© Fao L L
ee @ og L
a [ a=
ee r 7
« rod
TS T T T T
8 8g "ee eB 8

EP 1 75 SEP 27 75

16


-L

Appendix C: DMSP Electron and Optical Data

Ss
S

MAY

1S) 75

5.

8a,

53


Appendix C: DMSP Electron and Optical Data

Pn ow
Mra a

SPS

AUG 29 77

60


Appendix B: DMSP Optical Data

85,

ty 7
= b
Az’ +
2 L
a o
z L in
z L o oP
ze
r MB wo
L Bp
z ca
Ts Tow Tow Wf rel uJ To Tow Fr
& 8 BB é 8 & 6 B
JAN 27 75 FEB 23 75 MAR 22 75 APR 18 7S

33


Appendix B: DMSP Optical Data

a L L 4 L t 1 4 re L 4 L
Bag GB L A [ a) L 2 0 l@ L
0 Bey L ® [ © dy L Ole
POX L DM oF L Pn ote L o ot ol
Bagh 0 L Po | 2° L ” 4 L
° Bolan L Pana L arn Lp? wh on L
a
Pp L [ vz Pl ol on L
D » OL Deg, Mo L o L L
o>
oma heh L 2 00 Ban L » ol, a |
nse | A vup WW [ ” L E
ay L Gn Op L Pom) o 9 Lb o L
L L aw L ° L
a
PU L ARP L L ” L
2 L L L PB, wn L
L L wo G Dy L
L ” L L Man L
L L oO oe L PS Bor L
L L ° oe L ° va ol
L o L Pio | = PP Wo, L
Low HPD lo | ao [ 0 snd ol
in kv om L a) pn L FO OR L
are, L 2 Re lon L w oo Lb PB) oD L
Dip PD wo n no wn
> L L
” L ont D Mn) Rin w
° ban L ies Cod L on Bo L Oe Lb
L Py? dp L 2 Baro Lt 2 aw L
PO Ban L 2 sp L ap | L me Bh pe L
“ i. 2B Bin | on | AP L no PG L
Po Beppu ipa? oa
r pe Ze f
ao" 8 ag ¢ 8 B 2 € "7 8 a 2 g' 8 8
may 15 75 JUN 11 75 JUL 8 OS auG 4 75

34


Appendix C: DMSP Electron and Optical Data

L L 1 1 L a +
ER | op L Bugs .
i
Fin ‘5 L
oye | BS L
ate [ Bon? L
ht? ean Ta L
» far | “Be L
Ag | ° PB L
rin | OP ae |
@ ww
(Sao, | 0 Fry |
Ba | PO ep |
° ra L oB L
« FH, wl BHA oy [
Sip, ol Bin L
al
wo & | SPL
awn 2B an |
oy L oe L
mw
wo L no b
i L n L
o
wo a = wo =
on Dur [ L
e [ L
L Po B® L
° L O Boge L
= L OP rg, L
20? 4 oy, L ° Bp, L
8 Nao a 1a DH
g B a 8 zg 8 8
may 2 70 MAY 29 74

49


Appendix A: DMSP Electron Data

MAY

13°77

JUL

22


Appendix C: DMSP Electron and Optical Data

SL le NUr

ee 934

SL

@2@  Ybh

SL

Ydb

SL Bt

52



Appendix C: DMSP Electron and Optical Data

aa ¢

15
4

SEP 25 77

61




8S, -
J L
5 s
a § 5 Ss 35 L
-< Srey S58 gs s s 5 38s 85
55 9 £5% 3g eae
° 65 ? sg? Jae SS AS Ss 33s 8
aT i a
4 |
$
5S. OS a a i i 2
ms -
1 s r
2S . 3 5 33 SL
s 3
aE s > 5% ° : 8 [
° 5/8 $88 5,8) Sy Sis a, s 5 5
3 . 3 $
S
| L
Se Se
8s, -
> 734 $ 5 L
& |s.35s s 35 5
8 § 33. 5,585 5 5 s 3s ft
§s S .38 s s
vapa 3 SSE oes 9 372 os 8
~ ge 5h SSS
~ | &s 5 ~ 3 = Ss L
5 i OS SO i a A es a a ee TT
85, -
» Ms a L
o S$ i)
1.2% ¥ gs Sgs gs 8 5 8 si
s
Be 3 & é Say g§ es g§ &
~ > 3 g s S r
~ 5 $ S g 8
J 35 L
a

Appendix B: DMSP Optical Data



Appendix B: DMSP Optical Data

14 m Le et 1 er a oe 1
Zz br L
A Ze
Se [ 2 7s r ad Zz
zz L Fae L =
2 L 2 ee L al
A 2
= i 23a r # aL
sz ze = b eed
ae z iz
zz L Zz z= L Zz
eb Fz Re
ae r = = [ —
% L = L =
=e 2 = &*
za | = I ae
z L oa L zzz
& % L z Zz L z 2
= [ 24 [ Zz Zz
z Fe [ Zz ae = L zz
zzz | 2mm [ ww sS
ae 7 @ ze
z 22 z[ * Ze [
2 2% zz
L z L
Zz z= L i Bz
mF L L ZH =
Laéo
t ; z
Zz =
L 2
L Bz L ze
z [ 2 L 2
a= [ nl s
zz Ze #F
a r ““g wo T wv TS Ts uf Tod Td
~ o wi D o wo ao is)

BR ~
DEC 2 76 DEC 29 76 JAN 25 77

39



UAG-52

UAG-53

UAG-54

UAG-55

UAG-56

UAG-57

UAG-58

UAG-59

UAG-60

UAG-61

UAG~62

UAG-63

UAG-64

UAG-65

UAG-66

UAG-67

UAG-68

uAG-69

UAG-70

UAG-71

UAG-72

UAG-73

UAG-74

UAG-75

“Experimental Comprehensive Solar Flare Indices for Certain Flares, 1970-1974," by Helen W. Dodson and E.
Ruth Hedeman, McMath-Hulbert Observatory, University of Michigan Pontiac, MI, November 1975, 27 pp, $0.60.

“Description and Catalog of Ionospheric F-Region Data, Jicamarca Radio Observatory (November 1966 - April
1969), by N.L. Clark and T.£. Van Zandt, NOAA Aeronony Laboratory, Boulder, CO, and J.P. McClure, Univers ity
of Texas as Dallas, Dallas, TX, April 1976, 10 pp, $0.33.

“Catalog of Ionosphere Vertical Soundings Data," prepared by NOAA Environmental Data Service, Boulder, CO,
April 1976, 130 pp, $2.10.

"Equivalent lonospheric Current Representations by a New Method, Illustrated for 8-9 November 1969 Magnetic
Disturbances," by Y. Kamide, Cooperative Institute for Research in Environmental Sciences, University of,
Colorado, Boulder, CO; H.W. Kroehl, Data Studies Division, National Geophysical and Solar-Terrestrial Data
Center, Boulder, CO; M. Kanamitsu, Advanced Study Program, National Center for Atmospheric Research, Boulder,
CO; Joe Haskell Allen, Data Studies Division, National Geophysical and Solar-Terrestrial Data Center,
Boulder, CO; and S.- Akasofu, Geophysical Institute, University of Alaska, Fairbanks, AK, April 1976, 91 pp,
$1.60 (microfiche only).

“Iso- intensity Contours of Ground Magnetic H Perturbations for the December 16-18, 1971, Geomagnetic Storm,"
Y. Kamide, Cooperative Institute for Research in Environmental Sciences, University of Colorado, Boulder, CO,
April 1976, 37 pp, $1.39.

“Wanual on lonospheric Absorption Measurements," edited by K. Rawer, Institut fur Physikalische
Weltraunforschung, Freiburg, GFR, June 1976, 302 pp, $4.27.

"ATS6 Radio Beacon Electron Content Measurements at Boulder, July 1974 - May 1975," by R.B. Fritz, NOAA Space
Environment Laboratory, Boulder, CO, September 1976, 61 pp, $1.04.

“Auroral Electrojet Magnetic Activity Indices AE(11) for 1974," by Joe Haskell Allen, Carl C, Abston and
Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, December 1976, 144 pp,
$2.16.

"Geomagnetic Data for January 1976 (AE(7) Indices and Stacked Magnetograms)," by Joe Haskell Allen, Carl C.
Abston and Leslie 0. Norris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, July 1977,
57 pp, $1.07.

“Collected Data Reports for STIP Interval II 20 March - 5 May 1976, edited by Helen E. Coffey and John A.
McKinnon, World Data Center A for Solar-Terrestrial Physics, Boulder, CO, August 1977, 313 pp, $2.95.

"Geomagnetic Data for February 1976 (AE(7) Indices and Stacked Magnetograms)," by Joe Haskell Allen, Carl C.
Abston and Leslie 0. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, September
1977, 55 pp, $1.11.

"Geomagnetic Data for March 1976 (AE(7) Indices and Stacked Magnetograms),” by Joe Haskell Allen, Carl C.
Abston and Leslie 0. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, September
1977, 57 pp, $1.11.

“Geomagnetic Data for April 1976 (AE(8) Indices and Stacked Magnetograms)," by Joe Haskell Allen, Carl C.
Abston and Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, CO, February
1978, 55 pp, $1.00.

"The Information Explosion and [ts Consequences for Data Acquisition, Documentation, Processing," by G.K.
Hartmann, Max-Planck-Institut fur Aeronomie, Lindau, GFR, May 1978, 36 pp, $0.75.

“synoptic Radio Maps of the Sun at 3.3 mm 1970-1973," by Earle B. Mayfield and Fred I. Shimabukuro, Aerospace
Corp., El Segundo, CA, May 1978, 30 pp, $0.75.

“Lonospheric D-Region Profile Data Base, A Collection of Computer-Accessible Experimental Profiles of the D
and Lower E Regions," by L.F. McNamara, lonospheric Prediction Service, Sydney, Australia, August 1978, 30
pp, $0.88 (microfiche only).

"A Comparative Study of Methods of Electron Density Profile Analysis," by L.F. McNamara, Ionospheric
Prediction Service, Sydney, Australia, August 1978, 30 pp, $0-88 (microfiche only).

"Selected Disturbed D-Region Electron Density Profiles. Their relation to the undisturbed D region," by L.F.
McNamara, lonospheric Prediction Service, Sydney, Australia, October 1978, 50 pp, $1.29 (microfiche only).

“Annotated Atlas of the H-alpha Synoptic Charts for Solar Cycle 20 (1964-1974) Carrington Solar Rotations
487.1616," by Patrick S. McIntosh, NOAA Space Environment Laboratory, Boulder, CO, February 1979, 327 pp,
3.50.

“Magnetic Potential Plots over the Northern Hemisphere for 26-28 March 1976," A.D. Richmond, NOAA Space
Environment Laboratory, Boulder, CO; H.W. Krochl, National Geophysical and Solar-Terrestrial Data Center,
Boulder, CO; M.A. Henning, Lockheed Missils and Space Co., Aurora, CO; and Y. Kamide, Kyoto Sangyo
University, ‘Kyoto, Japan, April 1979, 118 pp, $1.50.

“Energy Release in Solar Flares, Proceedings of the Workshop on Energy Release in Flares, 26 February - 1
March 1979, Cambridge, Massachusetts, U.S.A.," edited by David M. Rust, American Science and Engineering,
Inc., Cambridge, MA, and A. Gordon Emslie, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, July
1979, 68 pp, $1.50.

“Auroral Electrojet Magnetic Activity Indices AE(11-12) for January - June 1975," by J.H. Allen, C.C. Abston, J.E.
Salazar and J.A. McKinnon, National Geophysical and Solar-Terrestrial Data Center, NOAA, Boulder, CO, August
1979, 114 pp, $1.75.

“ATS-6 Radio Beacon Electron Content Measurements at Ootacamund, India, October - July 1976," by S.D. Bouwer,
K. Davies, R.F. Donnelly, R.N. Grubb, J.£. Jones and J.H. Taylor, NOAA Space Environment Laboratory, Boulder,
CO, and R.G. Rastogi, M.R. Deshpande, H. Chandra and G. Sethia, Physical Research Laboratory, Ahmedabad,
India, March 1980, 58 pp, $2.50.

"The Alaska IMS Meridian Chain: Magnetic Variations for 9 March - 27 April 1978," by H.W. Kroehl and G.P. Kosinski,
National Geophysical and Solar-Terrestrial Data Center, Boulder, CO; S.-I Akasofu, G.J. Romick, C.E. Campbell and G.K.
Corrick, University of Alaska, Fairbanks, AK; and C.E. Hornback and A.M. Gray, NOAA Space Environment Laboratory,
Boulder, CO, June 1980, 107 pp, $3.00.



APPENDIX
Equatorial Latitude of Auroral Activity, 1972-77

The temporal variation of the equatorial latitude of the auroral ovals during the interval June 1972 - September
1977. The measurements are presented in 27-day Bartels seaments the first day of which is indicated on the
left. The vertical scale indicates invariant geomagnetic latitude. Optical measurements are indicated by the
letters N (north) and $ (south), and electron measurements are indicated by the letters A (north) and B

(south). Each point has been plotted approximately 1.4° higher in latitude than it should have been, and the
plotter saturated at latitudes less than 55° (see page 2 of text).



Appendix C: DMSP Electron and Optical Data

ai
o

O&C 31

4

51


Appendix C: DMSP Electron and Optical Data

;

a

un
Pn OA wr

Qe
of wo
on »

“A

o

no

o

o

o
o

ann

wD

‘A er0e,
fae
g a id

JUL 20 76

SS.

8a,

734

AUG

68

16

16

SS.

8,

T
fel
ne

SEP

12. 76

SS.

57


Appendix A: DMSP Electron Data

boa fl a \ fr a ee
2
© Mo Bee, L oe |
& fa [ oac
enn r ° a r ° Ee
ra
cr [ a one et L Op
Cee L wn L 0 ee
L « L o |S
L Gye L © of
a teow ac
L a.) L Fm
L 7 Ae L © coe
ced © ace}
L cay L ra
«
L oma F [ ©om
L ao gh L Om eg

og, Sr Or
L ry t oy
L pm s [ a
L ao « b a)
| a ne L o
a ar
L L « oe
i: er | Org L er
a L a Mx L 2° es
a 2 ey a eH
Bon 7 or a
a e rer 2 Eq
& L « hai ie t oft 05
x
Oey Be |B br eho b CORT py}
mm af fa om « mage
m, T [ oa = l - a
eS a |} — r & — Ty ae
wa a woud w w re) rel w wl
~~ ite o ~ wo ao ind oO ce

oe o
ocT 25 73 NOV 21 73 DEC 18 73 JAN 14 70

v1



WORLD DATA CENTER A
for
Solar-Terrestrial Physics

REPORT UAG-78

THE EQUATORIAL LATITUDE
OF
AURORAL ACTIVITY DURING 1972-1977

by

N.R. Sheeley, Jr. and R.A. Howard |

E.0. Hulbert Center for Space Research I

US Naval Research Laboratory Washington, DC 20375 |
I

and |
B.S. Dandekar

|
Air Force Geophysics Laboratory |
|

}
|

Hanscom AFB, MA 01731

October 1980 sil

Published by World Data Center A for
Solar-Terrestrial Physics, NOAA, Boulder, Colorado
and printed by

|
U.S. DEPARTMENT OF COMMERCE |
NATIONAL OCEANIC AND ATMOSPHERIC ADMINISTRATION I
ENVIRONMENTAL DATA AND INFORMATION SERVICE t
Boulder, Colorado, USA 80303 I

t

SUBSCRIPTION PRICE: $25.20 a year; $17.30 additional for foreign mailing; single copy price varies.*
Checks and money orders should be made payable to the Department of Commerce, NOAA/NGSDC.
Remittance and correspondence regarding subscriptions should be sent to the National Geophysical and
Solar—Terrestrial Data Center, NOAA, Boulder, CO 80303.


Appendix B: DMSP Optical Data

ne

32

SS.

&
D&C 31 74


Appendix A: DMSP Electron Data

8S

OEC 23 76

20


WORLD DATA CENTER A
National Academy of Sciences
2101 Constitution Avenue, N.W.

Washington,

D.C., U.S.A., 20418

World Data Center A consists of the Coordination Office

and seven Subcenters:

World Data Center A
Coordination Office
National Academy of Sciences
2101 Constitution Avenue, N.W.
Washington, D.C., U.S.A., 20418
[Telephone: (202) 389-6478]

Glaciology [Snow and Ice]:

World Data Center A: Glaciology
[Snow and Ice]

Inst. of Arctic & Alpine Research
University of Colorado

Boulder, Colorado, U.S.A. 80309
[Telephone: (303) 492-5171]

Meteorology (and Nuclear Radiation):

World Data Center A: Meteorology
National Climatic Center

Federal Building

Asheville, North Carolina, U.S.A.
[Telephone: (704) 258-2850]

Oceanography :

World Data Center A: Oceanography

National Oceanic and Atmospheric
Administration

Washington, D.C., U.S.A. 20235

[Telephone: (202) 634-7249]

Rockets and Satellites:

World Data Center A: Rockets and
Satellites

Goddard Space Flight Center

Code 601

Greenbelt, Maryland, U.S.A. 20771

[Telephone: (301) 344-6695]

NOTES:

Rotation of the Earth:

World Data Center A: Rotation
of the arth

U.S. Naval Observatory

Washington, D.C., U.S.A. 20390

[Telephone: (202) 254-4023]

Solar-Terrestrial Physics (Solar and
Interplanetary Phenomena, Ionospheric
Phenomena, Flare-Associated Events,
Geomagnetic Variations, Magnetospheric
and Interplanetary Magnetic Phenomena,
Aurora, Cosmic Rays, Airglow):

28801
World Data Center A
for Solar-Terrestrial Physics
Environmental Data and Information
Service, NOAA
Boulder, Colorado, U.S.A. 80303
[Telephone: (303) 499-1000, Ext. 6467]

Solid-Earth Geophysics (Seismology,
Tsunamis, Gravimetry, Earth Tides,
Recent Movements of the Earth's
Crust, Magnetic Measurements,
Paleomagnetism and Archeomagnetism,
Volcanology, Geothermics):

World Data Center A
for Solid-Earth Geophysics
Environmental Data and Information
Service, NOAA
Boulder, Colorado, U.S.A. 80303
[Telephone: (303) 499-1000, Ext. 6521]

1. World Data Centers conduct international exchange of geophysical observations
in accordance with the principles set forth by the International Council of Scientific

Unions. WDC-A is established in the
Academy of Sciences.

United States under the auspices of the National

2. Communications regarding data interchange matters in general and World Data
Center A as a whole should be addressed to: World Data Center A, Coordination Office

(see address above).

3. Inquiries and communications concerning data in specific disciplines should
be addressed to the appropriate subcenter listed above.


Appendix C: DMSP Electron and Optical Data

'
ae ngzz
an #2) =

7 [ zz"e

a L

vA
22 L
z L
= L
zz L
Wn Fz

zi L

o
22 L

oes z L

z
= 2B L
za
- |
2° Bn L
z 08 [
-e
CB zp PL
Zz
2z
& L
2 L
z lw zL 2
z

= Pe L

= OF le ZL
0 Fem oh

&
z2\ = OL
o

T T #2 uf uf

& B Bm & . ©

SEP 1S 72 oct 12 72

44


Appendix B: DMSP Optical Data

\ 14 \ \ 1 je ee ee ee t
oo PEP [ we L
2 Pho | ze L
0 BP on ao Zz L
0 bP | z = L
ren L L
% L L
® | ° z L
yl z B22
wow 3 r
ere re
ns °
zm? ae
B r wo % r
P wins eb L
wo ° ° z
an a | L a L
WH, in L L L
no B wow a
Naz r r r
=z
vim Bz! L os L = L
aD a a zz
z= r ” r 2 L
ny
° Bhim Bf t = r
on 2 Qo [ zoaz Ff
o
ren” L ai| L 2 L
za 2
Aa, L amp L L
© me i | ae
on [ “lB L 2 pe L
Ip
L ‘ifm | 2 |
L - zF = =
rn?
oe L 2 L
non bp 22
T 1 1 T T
ag @€ '¢  g¢ "4 "@ "xe "4 "8 "8B
sep ol 73 SEP 28 73 oct 25 73

28


no
1, Bp L 2 209 | m L Mn? bn L
Og L P apsrl L ° wo L wm L
por L eo OB L Yap L Ran L
5 Ce)
? un L BR] o L POR OF F pune O +
” L 2 Manos L 8 L oP Dan L
a Fo L HM |g L BID a L
DB ap L ely Fb ?agy L Pom L
20D) wo L ww L L bt
we | [ an Om [ nw [
# L ” L L Ba L
4 ae
= L nr L a L AP BPD L
& L n L a L an L
é ° L a L a L 9 o &a, L
& L a L 7 F nn +
A L apn L Pug b a ag L
an fw
FJ L on wn L O° DAB fa F
4
3 L Da L rw au L
a L wml L oan Ow O oy L
oO
< L | om L 2 24D 0 PD L
L ow nn aa | an PO L n PM wo lL
L PD? Wa L © ps9 In 7 PO? wh L
L a a) L 0 AR r B we L
° L moot Porosp L ne L
L “ a dil OMB ? pam 0 L
L aap a | Baka up Lb
w ny i
Lp HP In b oO on L Toy b
2, oe i a
1 r r 1 Arse | 1 ip r
ge “es "4 g 7s Tew gg g Te eg Be Te Ee

APR 3 «76 APR 30 76 MAY 27 76 JUN 23 76


Appendix A: DMSP Electron Data

8S

=, L a 4
a ae oe
age L =
2 enn L =m
L aoc ow
ore r ara = *
Ren L %
at we @
«c LL a i.
seg aoe
aT gd J g fe Ta
g 8B B88 g B B
AUG 29 77 SEP 25 77

23


ney

= HINO = +
DON = =
TNs ss Fe -NOOKW e+ + =
+O rps FONON + [NONI NOCMOOOD « > -

oe PS HONENON sNCLGONOGOOOH - OF +

wee NHOONN FIN sNOsNOMOs + = = -
Fo. 1 -NOOMONINNOsONUs0Ms0 -

BF FINOMOWU SO sSNINOHWW = +

> DDO OBOINNOOWING = + = =
ss FsOS0-++ ee

+785:

TIN DO TDF AOOONO= Ors eae ra :
cate (Oa OONOONAANNO - + > eee .
ce ee aa QUOOOsSIIMO ss e - ae ~ s
fiiit HG 5G OSGeo Ral lel:

Rina QOONR RNS SHO TERQNOHL OF DE ZAR MOR HOR HESTHONgHSHSHOONgE

RRR BTIPO VRANSS HO A SAQHSY HOF SRAKS IO” MRR RRSNOONAR AR EIOONRR

ARNT e ES ES SSH OS MUNUER E22 NOS WEWERE SSS euBouNaNeaERB2Oy

Be SES HES SES AHS SMRSU SEES AeA SESUERS SSI 2NeeERS YES SS 322%

OBES Teper ee oR NOs HBAs sy eZaSSONoR Soe gan
QaNoznecas Org DN SSSSIGSSISOOZRBARBERAB SOC BESBBSa
FLA AIRASHSSHSS— PV 'GGSISIFIAS— FHRSRISRIAG 1p BIRAGAS

mone -- Onn
WO + -mHnnn
WmMo- + nOnonoe
- +h Non -
ee eb +
+s pontmnoun -
+o e WMOON- n=
+ won -

+ pHvOONHHMHOm- o>

“DONS 0+ ++ enw:
a ee or.
DOMMMNO+ + + HOMn-
6+ O- OnEhrOonmum- --HHMOonMM-inews-
shee B+ NOUN + M-oHO+O-ud--w-
VOW SH IOFOHONG HVOF IN Fae OVOH-OFGeaOn
RRaeze RANSSLFHHQALL IPF HAART
S2PWHoSu aaa ee RIB UCOwMaNGa Tz 2OWOOw
SSPSEEES SARS SHNSHSESSI2AKSS
° ZOE esenae egongnzuen
Sant eeeoes HOMAISARVASRHROWMSRSSSLSSSS
HHRASSISRSS— A’ GISFAZAZATS

Plays of an index of lowest daily auroral
Patterns of

Y geomagnetic index C9 (ri

Comparison of 27-day Bartels dis
latitude (left) and the dail

Figure 1.

ght).

°
a
4
S
oO
g
3
s
&
2
8
2
=
S
g
an
3
25
+
52
on
2
~oO
7S
wow
uw
ot
os
>
3
ton
>t
we LO
Pi
on
g2
on
— 6
pe
wo
a
os
ow
=
3g
os
Fs
oP
or
Ow
co-
mil
gs
co
oe


Appendix C: DMSP Electron and Optical Data

APR 16 77 MAY 13° 77

59


Appendix C: DMSP Electron and Optical Data

T

65]

T
fa

JAN 28 (73

2 2n7
z= |
2 Be
a
22ge
Fas
- - ZZ.

rag
g 8

4 1
ra
o L
wn On
In b
BP is
nlto?
Ne OL
wo BD
AP [
0
nw r
wo |o r
. |
» L
on P
AL.
°D r
2 non
aN ted of
we (em 2f
vee
no m
is |
OBO P
222 om r
* onde * |
oo Ree lag [
o Pre
id Tw Mw
& 6 B
MAR 23° 73

45


Appendix C: DMSP Electron and Optical Data

a7


Appendix A: DMSP Electron Data
T

Cater r

oc
wd T
o

eS 6
MAR 23 73 auG =S 73 seP 1 73 SEP 28 73

ar re gd

w
o ite)

S
S
S.

65.

ita)

10