June

July

August

epnyj6u07 21ydesBoyay

of 096 oce 00 0Lz Ov ole o8l ost oz 06 09 Of O9e oe
nn Le ae | i an \
caves anos

i Ltpet Leet Brrel 4quON 7
ve sjsu
6z -TM~ —oet

ae 4

E 3 4
° jse.

-

- °

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6 8 fost
nh fee

L Guy 4

On

= 3 ey 4

L ol 4
6 ¢ dWWI 4u8W9dx3 TdW/NHE S 002

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L | UNONIS § 9) xn) B07 4
vee eS ey s soz

b sajonied ans6io0ug 4
et o0s< HX sre219-000's+ ge @ neO | SS Sloiz

+ o0s00z<  666'r00S-0- az@ AZO % J

r 002-05 p 66r-0010- gle NL oO “ay Dp |

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oe ose oe o0e Ole Ore Ole o8t ost oz 06 09 of o9e 0ce

€09L NOILVLOY — E61
LMWH ALIAILOY HWI0C

Day of Year

35


APPENDIX B

Solar Activity Charts, Rotations 1600-1611

31



8

epnyBu07 s1ydesBoyoH

November

December

O9e oce 00E Le Oz ole ogt ost oz 06 09 Oe 09 ore
T T T T T ~T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T T

iz giozi veoel gzazi anos 7]

r aun 7]
ote
se

TT 4
oe

L ° 4

Co ° mT jez

b 2 4

L oo 4

t 2 oes

L EE 4

L ety 4

"7

L ° Wey 4

8. see

L LC diNI awHEdx3 Jav/NHE 2 7

L naw 517-81 suoi01g Se 4

L 1 (AWS § 2tH9) xn 607 4

co ee ee ove

gee

C eet a

L. sajored a1.2610u3 4

LK 0s< X{ se1e219-000's-+ se@  neO sve

[  o0s-00z< 666’ 005-0 az @ Nz O J

L 00z-05 66r-0010- al © NEO > q

L g@— 6 4-'N- 2 o> 4

= ose

L oipey Aeu-X elegy °H

eet Pa Pe a a poy Pp
O9e Oce oo Le Ove Oz ogL ost oz 06 o9 of og oce

8091 NOLLW.LOY — E261
SLYVWHO ALIALLOV YV10S

Day of Year
40




UAG-27

AG-28

UAG-29

UAG-30

UAG-31

UAG-32

UAG-33

UAG-34

UAG-35

UAG-36

UAG-37

UAG-38

UAG-39

UAG-40

UAG-41

UAG-42

UAG-43,

UAG-84

UAG-45

UAG-46

UAG-47

UAG-48A,

uAG~49

UAG-50

UAG-51

uAG-52

UAG-53

“High Speed Streams in the Solar Wind," by D.S. Intriligator, University of Southern California, Los Angeles,
CA, dune 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. Norris, National Geophysical and Solar-Terrestrial Data Center, Boulder, C0, October 1973, 148 pp,
0.75.

“Catalogue of Data on Solar-Terrestrial Physics," prepared by NOAA Environnental Data Service, Boulder, C0,
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,

“synoptic Radio Maps of the Sun at 3.3 mm for the Years 1967-1969," by Earle B. Mayfield, Kennon P. lhite
III, and Fred I. Shimabukuro, Aerospace Corp., £1 Segundo, 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 D. 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 Weltraumforschung, 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
ATM-SKYLAB Missions," by R.F. Donnelly and E.L. Berger, NOAA Space Environment Laboratory; Lt. J.D. Busman,
NOAA Commissioned Corps; B. Henson, NASA Marshall Space Flight Center; T.B. Jones, University of Leicester,
UK; G.M. Lerfald, NOAA Wave Propagation Laboratory; K. Najita, University of Hawaii; W.M. Retallack, NOAA
Space Environment Laboratory and Wid. 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
gslie D. Worris, National Geophysical and Solar-Terrestrial Data Center, Boulder, 09, Decenber 1974, 142 pp,
0.75.

“Master Station List for Solar-Terrestrial Physics Data at WOC-A for Solar-Terrestrial Physics," by Rell.
Buhmann, orld 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 Haskel] Allen, Car] W. Abston and
Leslie D. Morris, National Geaphysteal and Solar-Terrestrial Data Center, Boulder, O), February 1975, 144 pp,
2.05.

“HeAlpha 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.

“HeAlpha 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 Nz, 10 Decenber 1971 through 21 March
1975," by Janes Us Warwick, George A. DUIk and Anthony C. Riddle, University of Colorado, Boulder, OD, Apr]
1975, 49 pp, $1.15.

“Catalog of Observation Times of Ground-Based Skylab-Coordinated Solar Observing Prograns," 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
WN. 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 bata 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, MD, 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, MJ. Koomen, D.J- Michels, Re
Tousey, C-R. Detwiler, D.E- Roberts, R.T. Seal, and J.D. Whitney, U.S. Naval Research Laboratory, Washington,
DC, and R.T. Hansen and $.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, CO,
August 1975, 125 pp, $1.85.

“High-Latitude Supplement to the URSI Handbook on Ionogram Interpretation and Rediction,” edited by W.R.
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 Spectrohelfograms from the Manned
Skylab Missions," by J.D. Bohlin and D.M. Rubenstein, U.S. Naval Research Laboratory, Washington, OC,
Novenber 1975, 30 pp, $0.54.

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

“Description and Catalog of lonospheric F-Region Data, Jicamarca Radio Observatory (Novenber 1966 - April
1969), by WL, Clark and T.E. Van Zandt, NOAA Aeronony Laboratory, Boulder, CO, and J.P. McClure, University
of Texas as Dallas, Dallas, TX, April 1976. 1 nm #33,





July

August

epmyBu07 s1ydesBoyoH

Oe 09e oce 00e Olt Ove rd o8t ost oz 06 of o9e oe
en ee | en T TT TTT
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r A@W S'b-8'L SUOIOId ——— 4
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y09l NOILV.LOY — EL6L
LYWHO ALIALLOW YW10S

Day of Year

36


I. CORONAL X-RAY STRUCTURE... 2...
Abstract... . 6.

1. Introduction. .....

CONTENTS

2. Synoptic Charts of X-ray Features from the Soft
X-ray Photographs Taken by the Skylab Experiment
S-054 (American Science and Engineering, Inc.) .

Acknowledgments... 2... 2%

Abstract

1. Introduction... ......

SOLAR FLARE ACTIVITY. . .

2. Procedure for Drawing Solar Activity Charts.

Acknowledgments... ee ee ee eee

REFERENCES .
APPENDIX Az
APPENDIX B:

Ha Synoptic Charts, Rotations 1601-1610

Solar Activity Charts, Rotations 1600-1611. .

31



Ha SYNOPTIC CHART
1974 - ROTATION I610

J2 t 28 et es a ka a 14 13S 2 “ w,9 8 7 6 ~ 5 4
worl 034 "033 032 031 030 029 * 28 "027 * 026 025 Yom 023 Om oar Ow "019 “ols “O17 "O16 015 om O13 uz rain to10 G09 008 * 007 * O06 * 005 * Os Dor

FEBRUARY, 1974 JANUARY, 1974

Note; Dashed lines r esent ct ections with sam
WEAK AND VARIABLE PATTERNS hed lines reiphetant connections itt

1 1 H H { 1

; .
330 0 30 60 90 120 150 180 210 240 270 300 330 360 30

! 29



Ha SYNOPTIC CHART

1973-ROTATION 1603

a7. 26 25 4 se al 8

330

5 4 0 2 ww. $ 8 7 6.5 4 3 2. 1 38 wb at
208° 207° 206 205. 20% 203° 202° 201 200" 199° 198° 197 196 "195 “1% ° 193° 192 "191 * 190° 189 187 a5 am pe a 0 179 78) Dor
Y, 1973
vue Rapid Evolution JUNE, 1973
+
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il eel ae “PC
=! rT | % -
| | al a — os
i h \ +| %&
rm 2 = — ~—>
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es T and +
= =
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-
$/10/74
| i —e f : i ae Lot Lt I
0 30 60 90 120 150 180 210 240 270 300 330 360 30

15



Ha SYNOPTIC CHART
1I973- ROTATION 1606

WW MW té £ 7 765 8 3 2 I HW Bb WN ve a
por ("290 "289 ° 288 * 287 285° 284° 283 m0 2m ae arr am as au 2 2m aT a m9 m8 267 BE * 265° Boh 263° 262 1201 * 260° | oY
OCTOBER, 1973 SEPTEMBER, 1973

a a OSE a

330 0 30 60 90 (20 150 180 210 240 270 300 330 360 30

ral



Ha SYNOPTIC CHART
1973-ROTATION 1604

23 22 UY O19 NW 6 nS MNS We NW $ 4 765 4S é LHI 29 2b aT “6

wor 235 °235 233° 232° 231 290229 228 227 206 m5 aah 223° 2m” ml’ 2 ag 28° 217° m6 21524 213 a2 al 20 209 208’ 207° 206 205 "| Dor
AUGUST, 1973 JULY, 1973

170

330 0 30 60 90 120 10 180 210 240 270 300 330 360 30

Vv







The result of all these inherent and subjective errors is that the results must be viewed as approximate.
This fact can be easily seen if one compares drawings showing photographs 105 and 106 at central meridian as shown
in Figure 2. The difference in central meridian is 12.8°. There are many similarities, but also many
differences, even though the photographs were taken only one day apart.

The photographs were fourth-generation prints. For photograph #63 and adjacent photographs, second-
generation prints were obtained from American Science and Engineering, Inc. As can be seen from Figure 3, which
compares the drawing made from (A) NSSDC 70-mm microfilm #63 with the drawing made from (B) AS&E 8" x 10" second-
generation negatives, the loop structure seen is more complex in the higher quality prints than in those used to
make these charts. However, the large scale structure is similar, and this was our main objective.

N

(B) $s

Fig. 2. Drawings of photograph 105, in (A), and 106, in {B), are compared. They have central meridians of
L=235.3° and L=222.5° respectively. Though taken only one day apart, the interpretations are different.

(A} s

Fig. 3. Drawings of X-ray structures made from NSSDC 70-mm microfilm #63, (A), and an 8" x 10" second-generation

negative of the same region, (B), show that although (A) shows fewer details, the large scale patterns
are similar.



) Ha SYNOPTIC CHART
1973, 1974 - ROTATION i609

550 29 28 eT 26 25 24.23, 22,21 19 8 wT Ss a 3 12 a 8 8?
001 305 364 363 «362 HHL HO 359358357 9586355

76 5 4 5 2.
007 006-005 Oh_- «003-02

JANUARY, 1974

\
270

L
240

27





SOLAR OBSERVATIONS DURING SKYLAB
APRIL 1973 - FEBRUARY 1974
I. CORONAL X-RAY STRUCTURE
II. SOLAR FLARE ACTIVITY

by

J. M. Hanson
Department of Aeronautical Engineering, University of Michigan
Ann Arbor, Michigan

. E. C. Roelof and R. E. Gold
Applied Physics Laboratory, The Johns Hopkins University
Silver Spring, Maryland

I. CORONAL X-RAY STRUCTURE
ABSTRACT

Large-scale (~ 10°) emission features visible in soft X-ray photographs from the American
Science and Engineering, Inc. (AS&) spectrographic telescope S-054 on Skylab have been
superposed on Hz Synoptic Charts [MeIntosh, 1975] for Carrington Rotations 1601 through
1610. The charts identify loop arcades and loop complexes associated with strong magnetic
fields, as well as coronal holes and areas devoid of emission loops. Although not
adequate for the study of the geometry of individual features, the charts convey a global
sense of coronal structure which is often difficult to obtain from individual (disk)
images.

1. INTRODUCTION

The interest of our group at the Johns Hopkins University/Applied Physics Laboratory in the American Science
and Engineering, Inc. soft X-ray images of the solar corona began with the first association of a solar wind
stream with a coronal hole photographed on a rocket flight in 1970 [Xmieger et al., 1973]. Later, the AS&E Skylab
data from the S-054 X-ray spectrographic telescope allowed us to extend the associations between coronal X-ray
structure and solar wind streams Piwveger et al., 1975; Nolte et al., 1971, Mitchell et al., 1980] and to include
energetic particles from 300 keV to > 3 GeV [Gold et al., 197%, b; Roelof et al., 197&, b; Roelof, 1976]. These
studies related interplanetary observations to large-scale X-ray features, e.g., coronal holes or large complexes
of loop-like structures. We decided that the next logical step was to make more detailed comparison with the
loop-like structures which spanned 5° or more of heliographic longitude or latitude.

We have therefore prepared an atlas of X-ray features from the S-054 Skylab data covering Carrington
Rotations 1601 - 1610 (May 29, 1973 to January 31, 1974). In order to facilitate comparison with other Skylab
data, we have mapped the X-ray features onto synoptic charts in heliographic longitude and latitude which overlay
the Ha Synoptic Charts of MeIntosh [1975]. We caution the user that, since we were initially interested in coarse
(v 10°) structure, we worked from positive prints made from 70-mm negatives available from the National Space
Science Data Center. These are of sianificantly lower quality than that available from AS&E internegatives,
as we document below. Even though individual loop locations and configurations cannot be considered exact,
we intend to use these X-ray synoptic charts as indicators of the general characteristics of regions of about 20°
x 20° in area. In other words, these charts can adequately identify loop arcades, loop complexes associated with
strong fields, and areas devoid of emission loops, but they are inadequate for any study of the geometry of
individual loops. We regard their main utility to be in conveying a global sense of coronal organization which is
difficult to gain from individual (disk) images. These charts are in Appendix A.

2. SYNOPTIC CHARTS OF X-RAY FEATURES FROM THE SOFT X-RAY PHOTOGRAPHS TAKEN BY THE SKYLAB EXPERIMENT S-054
(AMERTCAN SCTENCE AND ENGINEERING, INC.)

The basic data set was the 70-mm microfilm, (National Space Science Data Center, No. 73-027A-0513), from
which 8" x 10" glossy prints were made at two different exposures. These photographs covered Carrington Rotations
1601 - 1608, and those used are listed in Table 1 by numbers between 1 and 163. On rotations 1609 - 1610, the
S-054 images were partially obscured by a defective filter wheel, but usable images were provided on 8" x 10"
negatives by J. T. Nolte of AS&E. The out-of-focus image of the deformed filter wheel was clearly identifiable
and seriously affected only a portion of the image. Contact prints were made of these negatives, and those used
are listed by a 5-digit number in Table 1. A "montage" of the useful portions of the X-ray images from rotations
1609 and 1610 was published by Mitchell et al. [7980].

In order to use the photographs, the north and south poles of the Sun had to be located in each photograph.
The roll angle (Yp ) for the time when each picture was taken was found in the "Skylab X-Ray Telescope Film Image
Catalog" provided"by NSSDC with the documentation of the microfilm. Using a transparent overlay on the
Photographs, the poles were easy to locate. By centering the solar disk and aligning the lines with fiducial
marks on the left side of the photographs, Ypp located the north pole. In some photographs, fiducial marks did

not exist on the left side. In this case the marks on the right side were aligned with the result that Yrr gave
the south pole of the Sun.




Ha SYNOPTIC CHART
1973- ROTATION 1602
3029 2627 25 se to ea nS ae eS ak 2

por [isl “180 © 179" 178° 177 °1% ° 175° 174° 173° 172° 171 "1% ° 169‘ 168" 167 "166 ° 165 "164 ‘163 © 162° 161 ° 160 ‘159 158 "157 ° 15% 155 154 153 152 151 bor

JUNE, 1973 MAY ,1973

N70

Py

50

40

30

20

10
Eo

10

20

0

° +

50 ne

60 Po
$10

4/30/74

330 0 30 60 90 120 150 180 210 240 270 300 330 360 30



After the loops were picked out, they were traced on transparent acetate which was placed over the central
photograph. If the loops could be seen on the central photograph, they were drawn directly on the acetate. If
not, the Stonyhurst disks made it possible to find the latitudes and longitudes involved on adjacent images and

to relocate the loops on the drawing. In this manner, as many loops as possible were extracted from within 60°
of the sub-terrestrial point in the central photograph.

Using Stonyhurst disks, the footpoints of the loops were transferred from the acetate tracings to
the Ha Synoptic Charts from the Skylab Atlas by McIntosh [1975]. They were marked by dots and connected by lines
to show what loops exist. Again, if the exact locations of the footpoints are in question, the loops were
indicated by dotted lines. Certain areas of rotations 1603, 1608, and 1609 contain no data because of gaps in the
X-ray photographs.

Many possibilities for error exist in determining the loops. The error in locating the north and south poles
was less than 1/2 degree and was considered insignificant. The error in determining the longitude was at most
1/10 degree for rotations 1601 - 1608 and 1/2 degree for 1609 - 1610. The error from approximating By is less
than 1/2 degree for rotations 1601 - 1608, and less than one degree for 1609 - 1610. These errors are small and
random in nature. There are larger possibilities for error. Near central meridian, the error for locating
footpoints which can be seen is less than two degrees. Near the limb, however, the cosine projection effect
translates a small error in locating a loop into an error as large as five degrees in longitude near the limb,
although latitude is unaffected. Such near-limb images were used only as a last resort due to missing data.

There are also many subjective factors in defining the X-ray structures. Four examples of configurations
which could be misinterpreted are shown in Figure 1A, and the resulting drawings in Figure 1B. The chances of
these misinterpretations were minimized by using many photographs for the same region. This enabled the
structures to be viewed from different angles, reducing the chances for error. In example (i) of Figure 1, two
smal] loops, if unresolved, may be drawn as a single larger loop. On the other hand, a long loop (example ii)
whose top is not visible in emission may be drawn as two shorter loops. Example (iii) is a dark X-ray filament
channel which sometimes overlies a large Ha filament. Since high-lying loops are often faint, continuity could be
suggested and the full loops drawn, or conversely, the dark gap could be discernible with the same result as
example (ii). Finally, if there are loops near high latitudes which extend over the limb but are not fully
illuminated (example iv), only their lower segments may appear in the drawing.

N N

hu

( at filament

On ‘ w) . “

(B) $

Fig. 1. (A) shows four X-ray structures likely to be misinterpreted. (B) shows the resulting drawings. In
(i) two unresolved loops were combined; in (ii) the top of a loop is unseen and is drawn as two loops;

in (iii) a dark X-ray channel is interpreted as three complete loops; in (iv) unlit parts of a loop on
the limb are missed.

In addition, there will be one rather obvious situation where no loops will appear on the charts, although
they are likely to be present on the Sun. On the 64-second exposure negatives used for this study (NSSDC-73-027A-
05C/D), active region X-ray plages (which often overlie Hx plages) are strongly over-exposed. Therefore, end
points of loops leading into plages were not identifiable, nor were loops lying completely within large plages.
Consequently these charts depict only large-scale loops with at least one footpoint well away from bright X-ray
plage regions.

An independent problem was that in many cases there was evolution of the loop structure from day-to-day. The
result of this is that specific loops have to be chosen on a given photograph, while a day later the structure may
appear different on another photograph. This was especially apparent for parts of rotations 1609 and 1610.

3



Ha SYNOPTIC CHART
1973- ROTATION 1605

20.19 18 17 16 15 4 13,1 19 8 7 6 54a 21 a 50, 29, 28, 27, 6 25, 4 23, 22, 21 20

SEPTEMBER, 1973 AUGUST, 1973

——

2

$70 10$

Note: All loop foot-points west of 310° should be shifted 2° eastward,

Last Revision 9/10/77 PSM

Lop ett dt dt td dt dd tt
330 0 30 60 90 120 150 180 210 240 210 300 330 360 30

19


WORLD DATA CENTER A

for
Solar-Terrestrial Physics

REPORT UAG-79

SOLAR OBSERVATIONS DURING SKYLAB
APRIL 1973-FEBRUARY 1974
I. CORONAL X-RAY STRUCTURE

Il. SOLAR FLARE ACTIVITY

4
G SS
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December 1980



January

February

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O19L NOLLVLOY — PZ6L-EZ6L
SLYVHD ALIAILOV YVIOS

Day of Yoar

42


The data on the activity charts are accurate to approximately one degree and to two hours. The confirmed
visible flares, their X-ray data and their radio data were all found in Solar-Geophysical Lata (Comprehensive
Reports). The importance of the Hz flares is shown by the size of the circle. Bright flares are solid, while
normal and faint ones are open. The flares shown range in importance from importance (-) to importance 3. If
more than one flare occurred in the same active region within a two-hour interval, only the flare of highest
importance was plotted.

The number of the McMath Plage Region (MPR) containing the activity is indicated along the bottom of the chart,
with northern and southern latitude regions listed on two separate lines. Where more than one MPR occupies the
same longitude each additional region is coded with a different non-circular symbol.

The radio burst peak intensities are indicated by diagonal dashes emanating from each flare symbol. The
radio data considered were those from the essentially identical instruments at Sagamore Hill (Massachusetts) ,
Manila, the Canary Islands, and Athens. The frequencies used were 1415, 2695, 4995, and 8800 MHz. If the radio
data peaked within 10 minutes of the flare's Hz peak, they were considered. The radio flux shown on the activity
charts is the average over the Sous frequencies of the highest flux observed among the four observations at each
frequency. The flux is in W/LO°°m*Hz.

the 1-8 & x-ray fluxes were measured by the Solrad 9 or Solrad 10 spacecraft and reported in Solar—
Geophysical Data. The peak fluxes are indicated by horizontal or vertical dashes emanating from the flare
symbol. They are asgociated with a given flare if the peak in Hx and X-ray occurs within five minutes. Flux
units are ergs/10*cm*s. The three X-ray levels on the charts correspond to Boulder classifications M1-M4, M5-X4,
and >X5.

The connection longitude of the 1.8-4.5 MeV omnidirectional proton flux is shown on the activity charts. The
flux was measured by the JHU/APL energetic particle experiments on the IMP-7 and 8 spacecraft and is indicated at
the estimated high coronal "connection longitude". The connection longitude is the estimated source longitude of
the interplanetary plasma and “frozen in" interplanetary magnetic field, estimated using observed (1 hr. avg.)
solar wind velocities provided by the National Space Science Data Center from the MIT and LASL plasma instruments
on the same spacecraft [Nolte and Roelof, 1973]. The flux of the ~ 3 MeV protons is indicated by thg width of the
bar centered on the connection longitude path. It is measured to the nearest decade in particles/cm*s sr MeV.

ACKNOWLEDGMENTS.

We are grateful to J. Leighton and E. Heidgerd of the University of New Hampshire for their assistance in
preparing early versions of these charts. The charts, developed into their present form, constituted part of a
senior thesis presented by J.M.H. to the Department of Physics and Engineering of Loyola College (Baltimore).
Support for this work was provided by the NASA under Grant NSG-7055 and Air Force Geophysics Laboratory under Task
ZF10 via Navy Contract N00024-78-C-5384.

REFERENCES
BOHLIN, J. D. and 1975 "Synoptic Maps of Solar Coronal Hole Boundaries Derived
D. M. RUBENSTEIN from He II 304 Spectroheliograms from the Manned Sky-

lab Mission," Report UAG-51, (World Data Center A for
Solar-Terrestrial Physics, Boulder, Colorado, 80303).

soe Rene? 1974 nr Influence of Coronal Magnetic Structure on Low-

T. > nergy Solar Proton & " -

ELC. ROELOF, and ‘oy roton Events," Space Research XIV, 477-484.

R. REINHARD

GOLD, R. E., 1975a "Relation of Large-Scale Coronal X-ray Structure and

E. C. ROELOF, Cosmic Rays: 5. Solar Wind and Coronal Influence on a

J. T. NOLTE, and Forbush Decrease Lasting One Solar Rotation," Proc. 14th

A. S. KRIEGER International Cosmie Ray Conference (Munich), 3, 1095-
1100.

GOLD, R. E., 1975b "Relation of Large-scale Coronal X-ray Structure and

S. M. KRIMIGIS, Cosmic Rays: 3. Low-intensity Solar Particle Events with

E. C. ROELOF, Enhanced ~ 3 MeV Helium and Medium Fluxes Associated with

A. S. KRIEGER, and Solar Wind Streams," Proce, 14th International Cosmic Ray

J. T. NOLTE Conference (Munich), 5, 1710-1715.

KRIEGER, A. S., 1973 "A Coronal Hole and its Identification as the Source of a

A. F. TIMOTHY, and High Velocity Solar Wind Stream," Solar Phys., 29, 505-

E. C. ROELOF 525.

KRIEGER, A. S.5 1975 “Relation of Large-scale Coronal X-ray Structure and Cos-

J. T. NOLTE, mic Rays: 1. Sources of Solar Wind Streams and Ha Absorp-

P. S. MCINTOSH, tion features," Proc, 14th International Cosmie Ray

A. J. LAZARUS, Conference (Munich), 5, 1698-1703.

J. D. SULLIVAN,
R. E. GOLD, and
ROELOF



The X-ray structures, as drawn on a rectangular heliographic latitude and longitude grid, are printed in
color and overlaid on the Hz Synoptic Charts. When both loop footpoints were apparent, they were located by dots
and connected with a dashed line. If both footpoints could not be determined accurately, the minimum observed
extent of the loop was shown by a dotted line (as on rotation 1609).

The image resolution on rotation 1610 was also low, but for clarity, the loop connections are shown simply as
dashed lines. The strongly over-exposed images of X-ray plages (where no loops can be resolved) are indicated by
regions diagonally striped in color. The regions stippled in color are the coronal holes CH 1 through CH 6, taken
from Nolte et al., [1976b]. Boundaries for coronal holes not covered by that publication were taken from Bohlin
and Rubenstein, [1975], Areas not covered by either publication show no boundary data. The boundary of one
particularly extensive hole, extending from the south pole up past the equator in the eastern hemisphere on rota-
tion 1610 was estimated by MéteheZZ et al. [1980] from the same soft X-ray photographs listed in Table 1 and is
shown on the chart,

All-in-all, we believe that if the Synoptic Charts of X-ray features are regarded as what the eye perceives
in the X-ray photographs (and therefore as indicative only of the approximate location and nature of the actual
emission features), they will be useful as a representation of large-scale coronal structures. The synoptic .
charts should be considered as preliminary, but sufficiently accurate for use as they stand, within the guidelines
set down in the Introduction. Mote added in Proof’: Final cross-checking of the printed charts revealed two
regions of systematic misalignment, aside from isolated minor plotting errors (the great majority of which were
less than 2° in position). On rotation 1605, all footpoints west of 310° should be shifted 2° toward the east,
and on rotation 1608, al] footpoints between 120° and 350° should be shifted 2° to the west. These misalignments
are noted on the two charts.

ACKNOWLEDGMENTS

These charts constituted part of a senior thesis Presented by JMH to the Department of Physics and
Engineering of Loyola College (Baltimore). Full-sized originals of the Ha Synoptic Charts were provided by P. S.
McIntosh of the Space Environment Laboratory, NOAA/ERL. We appreciate the helpful comments of A. S. Krieger and
J. T. Nolte of American Science and Engineering, Inc. who also provided unpublished negatives to complement the
National Space Science Data Center 70-mm film record. Work at JHU/APL was supported by the National Aeronautics
and Space Administration under Grant NSG-7077 and by the Air Force Geophysics Laboratory via Task ZF10 of Contract
NO0024-78-C-5384 with the Department of the Navy.

II. SOLAR FLARE ACTIVITY
ABSTRACT

Charts of time versus longitude for each of Carrington Rotations 1600 - 1611 depict:
1) wi] importance, brightness, and location of confirmed flares; 2) peak flare X-ray flux
1-8 A; 3) peak flare decimetric radio intensity; and 4) flux of 1.8 - 4.5 MeV protons

plotted at their high coronal emission longitude estimated from simultaneously measured
solar wind velocity.

1, INTRODUCTION

These Solar Activity Charts are a compilation for the Skylab period of selected indices of optical solar
flares, radio bursts, soft X-rays, and energetic particles in a concise form. The charts were initially designed
to complement studies of the coronal and interplanetary distribution of energetic solar particle populations,
although their compact representation of spatial and temporal relationships has been of assistance in a wide
variety of solar-terrestrial studies. The charts show the Hz importance and brightness of confirmed flares, the
1-8 A peak X-ray flux and a spectral average of decimetric radio emissions related to the optical flares. Full
disk coverage extends from April 13, 1973 through February 24, 1974. See Appendix B.

The energetic particle fluxes are represented on the charts as a continuous swath centered on the estimated
high coronal connection longitude of the large scale interplanetary field line from Earth. The width of the swath
is proportional to the logarithm of the ~ 3 MeV proton flux measured at Earth. The charts are organized in
heliographic longitude versus time so it is easy to follow the development of an active region throughout its disk
Passage on a given solar rotation as well as its recurrences over several rotations, since all the activity from a
given region falls on a straight vertical line. Conversely, all the flares and related radio and X-ray bursts on
the disk at a given time are distributed along a horizontal line. The charts also indicate directly the distance
between an active region and the longitude where energetic protons (associated with activity in that region) were
injected onto the interplanetary field lines leading to the Earth.

2. PROCEDURE FOR DRAWING SOLAR ACTIVITY CHARTS

On the Solar Activity Charts for Carrington Rotations 1600 - 1611, time is measured on the vertical axis and
heliographic longitude on the horizontal axis. Time progresses upward and is measured in day of year on the left
and day of month on the right. Thus the locus of each limb progresses from lower right to upper left. The format
follows that introduced by cold et al. [1974].



September

October

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ew

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9091 NOLLV.LOW — E261
LYVHO ALIALLOV YV10S

Day of Year

38




January

February

March

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0 T TT T Teo
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LI9L NOLLW.LOY — PZ6L
LYWHO ALIAILOV YV10S

Day of Year

43


“WOE

“W398

345 344 3433423340

bor

|

DECEMBER 1973

76,5 4 J

339-338

337

_2
336 335

/ 50

334

Ha SYNOPTIC CHART
1973 -ROTATION 1608

29,2627, 26,25, 24,23, 22 a.

p MW Ns
333-3323 330 329 728 e736 325 * 324 * 323 ! :

0 |

50
|

“ i 4“*\ -\* i sf Bo
30} Sea =r

ss
a ae

——

Note: All loop foot-points 126°—350° should be shifted 2° westward.
. 10/15/74,
L —— 1 it = i i ol | Cs es a es | | | | | | | 1 it | |
330 0 30 60 90 120 150 180 210 240 270 300 330 360 30

25


From the time of the day when the picture was taken, the heliographic longitude of central meridian could be
calculated. These longitudes are listed (by photograph number) in Table 1. Stonyhurst Sun disks (transparent
overlays) for integer values of the inclination (By) of the solar equator were laid over the photograph and the
latitudes and longitudes read directly.

For each area of the Sun during rotations 1601 - 1608, photographs were examined and those in which the
region of interest was most clearly shown were chosen. This choice generally included two or three photographs
taken before and two or three taken after the main photograph. The different photographs made it possible to view
the area of interest in the corona from many different angles. Viewing different photographs made it possible to
discern what three-dimensional loops existed and to pick out many that were not visible in the central
photograph. Only the central photographs are listed in Table 1.

TABLE 1

PRINCIPAL X-RAY PHOTOGRAPHS USED FOR CHARTS

Carrington Heliolongitude Time of Photo
Photo No. Rotation of CM (deg) (day :hr:min)
1 1601 46 14!
5 1602 352 15.
7 1602 263 161
ll 1602 210
7 1602 120
20 1602 85
24 1602 32
28 1603 339
33 1603 272
38 1603 206
44 1603 128
46 1604 314
52 1604 239
56 1604 176
63 1604 77
73 1605 312
81 1605 206
91 1605 73
97 1606 353
99 1606 327
101 1606 288
105 1606 235
106 1606 222
115 1606 104
116 1606 90
120 1606 37
125 1607 332 201:
127 1607 298 293:14:06
136 1607 186 302:01:40
144 1607 81 310:02:12
149 1607 15 315:01:53
153 1608 303 320:12:14
155 1608 262 323:14:46
163 1608 164 331:01:43
050048 1609 140 360:05:23
051039 1609 96 363:13:41
051544 1609 17 4:12:37
052095 1610 285 11:14:03
053275 1610 207 17:14:39
054996 1610 154 21:12:08
056362 1610 75 27:14:12
056542 1610 22 31:13:05

During rotations 1609 and 1610, the out-of-focus image of a bent filter wheel caused part of each photograph
to be obscured. For this reason, the procedure was modified slightly. Starting with the earliest chosen
photograph, loops seen on each photograph were extracted. These loops were checked with the other photographs.
The photographs were studied in the order of when they were taken.

For the entire period, the loops chosen were those in which both footpoints could be seen. When both
footpoints were apparent, they were located by dots and connected with a dashed line. If both footpoints could
not be determined accurately, the minimum observed extent of the loop was shown by a dotted line. This was done
so that at least an idea of the structure involved could be obtained (e.g., Rotation 1609).





April

May

June

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T T T T T T T T T T T T T T T T T T T T T T T T T T T TT T T T T T T T T T
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LO9L NOLLW.LOW — E261
LYVHO ALIALLOW YV1OS

Day of Year

33


June

July

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2091 NOLLV.LOH — E261
LYWHO ALIALLOV YV1OS

Day of Year

34






December

January

a

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st

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6091 NOLLW.LOY — €Z6L
LYVHO ALIALLOV YV1OS

Day of Yoar

41


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4091 NOLLW.LOY — e261
LYVHO ALIALLOV YVWT1OS

Day of Year
39


APPENDIX A
Ha Synoptic Charts, Rotations 1601-1610



Ha SYNOPTIC CHART
1973- ROTATION 1601

32 1 3 30 29 28 a7 6 5 he ss ee a aa] ee BT
Dor [ase “as0 arn isi 150 us ua *ur tus Pus ms tus "442 a uo Us. 18 137 "1% 335 1% 133 2 iat 130 "129 * 128 War a6 *aa5 aa, aaa Dor
JUNE, 1973 MAY, 1973
= SS wn
ol — 60
‘ ars i ani =-—|\— +
50 (t+ it Mn gm | |_| * Isp
mK q ce J - ) fre - - 7 - 4
Oly tes tte To er TP aL Ay 40
30 4 =| ro he fy
C IL —. web]. +
To]

Qs

10S

n/a,
A ee DO DO DG CG DC
120 150 180 210 240 270 300 330 360 30

ll



WORLD DATA CENTER A
for
Solar-Terrestrial Physics

REPORT UAG-79

SOLAR OBSERVATIONS DURING SKYLAB
APRIL 1973-FEBRUARY 1974
I. CORONAL X-RAY STRUCTURE
li. SOLAR FLARE ACTIVITY

by

J.M. Hanson
Department of Aeronautical Engineering, University of Michigan
Ann Arbor, Michigan

E.C. Roelof and R.E. Gold
Applied Physics Laboratory, The Johns Hopkins University
Silver Spring, Maryland

vill
December 1980

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
ENVIRONMENTAL DATA AND INFORMATION SERVICE
Boulder, Colorado, USA 80303

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.

*Price this issue $2.50.



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T T T T T T T T T T T T T T T T T T T T T
1s T T TT T T T T T T T T
L o0ezt 90ez1 ezezh
veeet weet
L °°
5
| E
| oL

3 Ss

BOL

< she
dl oe
stp
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06 L
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0091 NOLLV.LOY — 261
LYWHO ALIALLOW YW10S

Day of Year
32




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]: Rotation of the Earth:
World Data Center A: Glaciology World Data Center A: Rotation
[Snow and Ice] of the Earth
Inst. of Arctic & Alpine Research U.S. Naval Observatory
University of Colorado Washington, D.C., U.S.A. 20390
Boulder, Colorado, U.S.A. 80309 [Telephone: (202) 254-4023]

[Telephone: (303) 492-5171]
Solar-Terrestrial Physies (Solar and

Meteorology (and Nuclear Radiation): Interplanetary Phenomena, Ionospheric
Phenomena, Flare-Associated Events,
World Data Center A: Meteorology Geomagnetic Variations, Magnetospheric
National Climatic Center and Interplanetary Magnetic Phenomena,
Federal Building Aurora, Cosmic Rays, Airglow):
Asheville, North Carolina, U.S.A. 28801
[Telephone: (704) 258-2850] World Data Center A
for Solar-Terrestrial Physics
Oceanography : Environmental Data and Information
Service, NOAA
World Data Center A: Oceanography Boulder, Colorado, U.S.A. 80303
National Oceanic and Atmospheric {Telephone: (303) 497-6323]
Administration
Washington, D.C., U.S.A. 20235 Solid-Earth Geophysics (Seismology,
[Telephone: (202) 634-7249] Tsunamis, Gravimetry, Earth Tides,
Recent Movements of the Earth's
Rockets and Satellites: Crust, Magnetic Measurements,
Paleomagnetism and Archeomagnetism,
World Data Center A: Rockets and Volcanology, Geothermics) :
Satellites
Goddard Space Flight Center World Data Center A
Code 601 for Solid-Earth Geophysics
Greenbelt, Maryland, U.S.A. 20771 Environmental Data and Information
[Telephone: (301) 344-6695] Service, NOAA
Boulder, Colorado, U.S.A. 80303
[Telephone: (303) 497-6521]
NOTES:

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 United States under the auspices of the National
Academy of Sciences.

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.







August

September

epnyBu0q o1ydesBoyaH

of 09 oe 00e x4 Ove ra ost Ost ozt 06 09 of ose oct
T T T T T T T T T TOT T T T T TT TT. T T T T T T T T T T T T T T T T T T T T sez
[ gavel covet beset voszt ziszt eset wanos |
Loset toszt ose, «est won,
~ zszl 7
at Joce
& ez
- =~ 4
SS
SS 5 4
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L a 4
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at 1— (AW as § 29) xnyj 607 sss
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ah ouz
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oe O9e o8e 008 uz ove o1z ost ost oz 06 09 oF 098 ee

GO9L NOLLV.LOY — E261
LYVHO ALIALLOV YV1OS

Day of Year

37


Ha SYNOPTIC CHART
1973-ROTATION 1607

WS EWM WG O76 SF 6 FI 2 MH HAMA UNUVNMKABAUA 2d BAA NW WW iuitis
oY 311 © 310 © 309 * 308 © 307 “308 “305 “304 ~ 303" 302 301 300 299 208 297 29% 295 2M é «293° «29% «291 «290 289 «288287 wr

NOVEMBER, 1973 OCTOBER, 1973

330 0 30 rr) r) 120 0 190 20 240 210 "30 330 30 30

23



MCINTOSH, P. S.

MITCHELL, D. G.,

E.
J.

C. ROELOF, and
H. WOLFE

NOLTE, J.T. and
E.C. ROELOF

NOLTE, J. T.,

A.

S. KRIEGER,

F. TIMOTHY,

E. GOLD,

C. ROELOF,
VATANA,

J. LAZARUS,

D. SULLIVAN, and
S. MCINTOSH

NOLTE, J. T.,

A
AL
G.
Mw

S. KRIEGER,
F, TIMOTHY,
S. VAIANA, and
V. ZOMBECK

ROELOF, E. C.

ROELOF, E. C.,

Ss.
A.
Jd.
Pp,
AL
a.

E, GOLD,

M,. KRIMIGIS,
S. KRIEGER,

T. NOLTE,

+ MCINTOSH,

. LAZARUS, and
» SULLIVAN

oan

ROELOF, E. C.,

R.

>

J.
De.

E. GOLD,
S. KRIEGER,
T. NOLTE, and
VENKATESAN

1975

1980

1973

1976a

1976b

1976

1975a

1975b

"H-alpha Synoptic Charts of Solar Activity for the Period
of Skylab Observations May 1973 - March 1974, Report UAG-
40, (World Data Center A for Solar-Terrestrial Physics,
Boulder, Colorado, 80303).

"Latitude Dependence of Solar Wind Velocity Observed 2 1
AU," J. Geophys. Ree., 85, (in press).

"Large-Scale Structure of the Interplanetary Medium,"
Solar Phys., 83, 241-257.

"Coronal Holes as Sources of Solar Wind," Solar Phys.,
46, 303-332.

"An Atlas of Coronal Hole Boundary Positions, May 28 to
November 21, 1973," Solar Phys., 46, 291-301.

"Solar Particle Emission," in Phystes of Solar Planetary
Envivonnents, Proce. of the International Symposiun on
Solar-Terrestrial Physics (Boulder), D. J. Williams, Ed.
(American Geophysical Union, Washington, D. C.), 1, 214-
231.

“Relation of Large-scale Coronal X-ray Structure and
Cosmic Rays: 2. Coronal Control of Interplanetary In-
Jection of 300 keV Solar Protons," Proc. 14th Interna~
tional Cosmic Ray Conference (Munich), 5, 1704-1709.

"Relation of Large-Scale Coronal X-ray Structure and Cos-
mic Rays: 4. Amplitude of the Diurnal Variation in Neu-
tron Monitors on Interplanetary Field Lines Originating
Above Coronal Holes," Proc. 14th International Cosmic Ray
Conference (Munich), 4, 1138-1143.



UAG SERIES OF REPORTS

Between 6 and 12 UAG Reports are published at irregular intervals each year. Subscriptions may be ordered through the
National Geophysical and Solar-Terrestrial Data Center, Environmental Data and Information Service, NOAA, Boulder, CO

80303, USA.

The annual subscription price is $25.20 ($17.30 additional for foreign mailing). Each year the single copy

prices total less than $25.20, the expiration data for all subscriptions will be extended. Back issues may be purchased at
the prices shown below plus a'$3.00 handling charge per order; some reports, though, are available only on microfiche.
Orders mist include check or money order payable in U.S. currency to the Department of Conmerce, NORA/NGSDC.

UAG-1

URG-2

UAG-3

uAG-4

UAG-5

UAG-6

UAG-7

UAG-8

UAG-9

UAG-10

UAG-12

UAG-13

UAG-14

UAG~16

UAG-17

UAG-18

UAG-19

UAG-21

AG-22

UAG-23

UAG-23A,

UAG-24

UAG-25

UAG-26

“IQSY Night Airglow Data," by L.L. Smith, F.E. Roach, and J.M. McKennan, ESSA Aeronomy Laboratory, Boulder,
0, July 1968, 305 pp, $1.75.

“A Reevaluation of Solar Flares, 1964-1966," by Helen li Dodson and E. Ruth Hedenan, Melfath-Hulbert
Observatory, University of Michigan, Pontiac, MI, August 1968; 28 pp, $0.3

“Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-41 MHz, 6 July 1966 through 8 Septenber
1968," by James W. Warwick and George A. Dulk, University of Colorado, Boulder, CO, October 1968, 35 pp,
$0.55.

“Abbreviated Calendar Record 1966-1967," by J. Virginia Lincotn, Hope I. Leighton and Dorothy K. Kropp, ESSA
now NOAA, Aeronony and Space Data Center, Boulder, CO, January 1969, 170 pp, $1.25.

“Data on Solar Event of ay 23, 1967 and its Geophysical Effects," compiled by J. Virginia Lincoln, World
Data Center A, Upper Atmosphere Geophysics, ESSA now NOAA, Boulder, CO, February 1969, 120 pp, $0.65.

“International Geophysical Calendars 1957-1969," by Asi. Shapley and J. Virginia Lincoln, ESSA Research
Laboratories, now NOAA, Boulder, CO, Narch 1969, 25 pp, $0.30.

“Observations of the Solar Electron Corona: February 1964 - January 1968," by Richard T. Hansen, High
Altitude Observatory, NCAR, Boulder, CO, and Kamuela, HI, October 1969, 12 pp, $0.15.

"Data on Solar-Geophysical Activity October 24 - November 6, 1968," Parts 1 and 2, compiled by J. Virginia
Lincoln, World Data Center A, Upper Atmosphere Geophysics, ESSA now NOAA, Boulder, CO, March 1970, 312 pp,
$1.75 (includes Parts 1 and 2).

"Data on Cosmic Ray Event of Novenber 18, 1968 and Associated Phenomena," compiled by J. Virginia Lincoln,
World Data Center A, Upper Atmosphere Geophysics, ESSA now NOAA, Boulder, CO, April 1970, 109 pp, $0.55.

“Atlas of Ionograms," edited by A.H. Shapley, ESSA Research Laboratories now NOAA, Boulder, CO, May 1970, 243
pp, $1.50.

"Solar-Geophysical Activity Associated with the Major Geomagnetic Storm of March 8, 1970," Parts 1, 2 and 3,
compiled by J. Virginia Lincoln and Dale B. Bucknam, World Data Center A, Upper Atmosphere Geophysics, ESSA’
now NOAA, Boulder, CO, April 1971, 466 pp, $3.00 (includes Parts 1-3).

"Data on the Solar Proton Event of November 2, 1969 through the Geomagnetic Storm of Novenber 8-10, 1969,"
compiled by Dale 8. Bucknam and J. Virginia Lincoln, World Data Center A, Upper Atmosphere Geophysics, ESSA
now NOAA, Boulder, CO, May 1971, 76 pp, $0.90.

“An Experimental, Comprehensive Flare Index and Its Derivation for 'Major" Flares, 1955-1969," by Helen W.
Dodson and. Ruth Hedenan, NcMath-Hulbert Observatory, University of Michigan, Pontiac, MI, July 1971, 25
pp, $0.30.

“Temporal Development of the Geophysical Distribution of Auroral Absorption for 30 Substorm Events in each of
19SY (1964-65) and TASY (1960)," by F.T. Berkey, University of Alaska, Fairbanks, AK; VM. Driatskiy, Arctic
and Antarctic Research Institute, Leningrad, USSR; K. Henriksen, Auroral Observatory, Tronson, Norway D-H.
Jelly, Communications Research Center, Ottawa, Canada; T.I. Shchuka, Arctic and Antarctic Research Institute,
Leningrad, USSR; A. Theander, Kiruna Geophysical Observatory, Kiruna, Sweden; and J. Yliniemi, University of
Oulu, Oulu, Finland, September 1971, 131 pp, $0.70 {microfiche only).

“Jonospheric Drift Velocity Measurements at Jicamarca, Peru (July 1967 - March 1970)," by Ben 8. Balsley,
NOAA Aeronony Laboratory, Boulder, C0, and Ronald F. Woodman, Jicamarca Radar Observatory, Instituto
Geofisico del Peru, Lima, Peru, October 1971, 45 pp, $0.55 (microfiche only).

"A Study of Polar Cap and Auroral Zone Magnetic Variations," by K. Kawasaki and S.-I. Asasofu, University of
Alaska, Fairbanks, AK, June 1972, 21 pp, $0.20.

"Reevaluation of Solar Flares 1967," by Helen W. Dodson and E. Ruth Hedeman, McMath-Hulbert Observatory,
University of Michigan, Pontiac, MI, and Marta Rovira de Miceli, San Miguel Observatory, Argentina, June
1972, 15 pp, $0.15.

“preliminary Compilation of Data for Retrospective World Interval July 26 - August 14, 1972," by J. Virginia
Lincotn and Hope 1; Leighton, World Data Center A for Solar-Terrestrial Physics, NOAA, Boulder, CO, Novenber
1972, 128 pp, $0.70.

“Auroral Electrojet Magnetic Activity Indices (AE) for 1970," by Joe Haskell Allen, National Geophysical and
Solar-Terrestrial Data Center, Boulder, CO, November 1972, 146 pp, $0.75.

"U.R«S.I. Handbook of Ionogram Interpretation and Reduction," Second Edition, November 1972, edited by W.R.
Piggott, Radio and Space Research Station, Slough, UK, and kK. Rawer, Arbeitsgruppe fur Physikalische
Weltraumforschung, Freiburg, GFR, November 1972, 324 pp, $1.75.

"U.R.S.1. Handbook of Ionogram Interpretation and Reduction,” Second Edition, Revision of Chapters 1-4,
edited by W.R. Piggott, Radio and Space Research Station, Slough, UK, and K. Rawer, Arbeitsgruppe fur
Physikalische Weltraumforschung, Freiburg, GFR, November 1972, 136 pp, $2.14.

“ata on Solar-Geophysical Activity Assoctated with the Hajgr Ground Level Cosmic Ray Events of 28 January
and 1 Septenber 1971," Parts 1 and 2, compiled by Helen E. Coffey and J. Virginia Lincoln, World Data Center
A for Solar-Terrestrial Physics, NOAA, Boulder, CO, December 1972, 462 pp, $2.00 (includes Parts 1 and 2).

“Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-41 Miz, 9 Septenber 1968 through 9
December 1971," by James W. Warwick, George A. Dulk and David G. Swann, University of Colorado, Boulder, CO,
February 1973, 35 pp, $0.35.

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



UAG-54

UAG-55

UAG-56

UAG-57

UAG-58

UAG-59

UAG-60

UAG-61

UAG-62

URG-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

UAG-76

UAG-77

UAG-78

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

“Equivalent Ionospheric Current Representations by a New Method, IIlustrated for 8-9 Novenber 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,
C0; Joe Haskell Allen, Data Studies Division, National Geophysical and Solar-Terrestrial Data Center,
Boulder, CO; and S.-I 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 Decenber 16-18, 1971, Geomagnetic Stomn,"
Y. Kamide, Cooperative Institute for Research in Environmental Sciences, University of Colorado, Boulder, CO,
April 1976, 37 pp, $1.39.

“Manual on Ionospheric Absorption Measurements," edited by K. Rawer, Institut fur Physikalische
Weltraumforschung, 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, Septenber 1976, 61 pp, $1.04,

“Auroral Electrojet Magnetic Activity Indices AE(11) for 1974," by doe Haskell Allen, Carl C. Abston and
Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center, Boulder, C0, December 1976, 144 pp,
$2.16.

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

“Collected Data Reports for STIP Interval II 20 March - § 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 D. Worris, Rational Geophysical and Solar-Terrestrial Data Genter, Boulder, CD, Séptenber
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, ational Geophysical and Solar-Terrestrial Data Center, Boulder, CO, Septenber
1977, 57 pp, $1.11.

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

“The Information Explosion and Its 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 mn 1970-1973," by Earle B. Mayfield and Fred I. Shimabukuro, Aerospace
Corp., ET Segundo, CA, May 1978, 30 pp, $0.75.

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

“A Comparative Study of Methods of Electron Density Profile Analysis," by LeF. 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, Tonospheric 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
1487-1616," 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. Kroehl, 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 (microfiche only).

“Auroral Electrojet Magnetic Activity Indices AE(11-12) for January - June 1975," by J.H. Allen, C.C. Abston, J.E.
Salazar and Joke Mckinnon, atonal 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, ReN. Grubb, J.E. Jones and J.H. Taylor, NOAA Space Environment Laboratory, Boulder,
CO, and R.G. Rastogi, H.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.

“Auroral Electrojet Magnetic Activity Indices AE(12) for July - December 1975," by J.H. Allen, C.C. Abston, J.E.
§glezar and.d-A. Mekinnon, National Geophysical and Solar-Terrestrial Data Center, NORA, BouTder, C0, August 1980,
116 pp, $2.50.

“synoptic Solar Magnetic Field Maps for the Interval Including Carrington Rotations 1601-1680, May 5, 1973 - April
26, 1979," by J. Harvey, B. Gillespie, P. Miedaner and C. Slaughter, Kitt Peak National Observatory, Tucson, AZ,
August 1980, 66 pp, $2.50.

“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, U.S. Naval Research Laboratory, Washington, DC and B.S. Dandekar, Air Force Geophysics
Laboratory, Hanscom AFB, MA, October 1980, 61 pp, $3.00.