ane ony ony
zm @ we w@ 8 vw L 2 € F § 9 g£ 8 6 oo ht wo & om ss om a om a oo ye
ce pe tt Pp et ee oe PP rot op ee
o- or
oe A oe-
- 6°S vf -
02" f e ”
Lid \ 27 Ko Sef
om * a-
x
Mod x x ~ x (a Ms oo a
(ry 4 o= ¥ ab
" ‘€y TH g <The) ao 4a} —| 01
a |} Roe |G | Ns ¢> rid.
" 2
ow Vauane re 7 o
0c oe
o +o
09 Ove oe 00E 087, 09 Oe Oz 002 OBL OL Ort oz 001 og 09 or 4 00
2681 NOLLVLOW 8961
nar ane an
4 ETA ra Of t a € v s 9 ra 8 6 OL u a eb wm st mn at 8L 6L 02 Ww a & c4 st
coe ee ee ee ee pe tg ee pw
o- or
|~le |
oe- y) e. 5 — oe
we - am 9°, Rae A w-
im VA ¥ | 24 R i tT fr
> . 7 x o1-
ep Ce a6 x yl x VF
‘Mod of 3
o us ay PN + Ql on
v5 3 7, 3
" ° a ; ve 2
a Be (e) @ (Ast 4 eseply | oh ER
QC Ni ak ( | "
r
I Of
or or
0096 Ove Ore 00 087 09% Ove zz 002 st Om OrL ozt 00L oe oe ow 4 0

9€S1 NOLLV.LOY 8961

16


GEG] UONDJOY 40} BIqQD|IDAY DJDG ON

ony d3s
9 Z 8 OL u a el mn st Tt a aL 6L oz Ww 4 & 4 st we a @ 4 of te t
oe moe ae ae oye ye ye ip ie eee ° oe
or
LH Le] N
oe~ ¥. <—e? a
. YS =) aan)
oa- io" Xe? Ny,
ov oa
ol- 4
[ x a x
‘Mod x
cal x px = ee

oO

i" =f (( pte | “ele Cite)
w@ 8s T

¥ q

“KE SLES WEY

i exu ae
o

009E Ore Oe 00€ 08z 09% 4 0 002 ot om Ort oz 00t oF 09 oO 02

2S1 NOLLVLOY - 2961

10



ay
@ 6 oF tf @ el + sh of 2b gt GL o2 i 2 t ve Se 92 22
sop ot tye ee ee eee ee ee

ty x oe
29
|x |_| Ge mail f
| x a i gh. xX 1x
I CA

—9 0%? ig

(0
Hip
P(
Tey
Bi
Ne
Ly

2 se 41
el [J or] NE
oF
oe S~SCSSCSCSCSC~ SSCS SSCS 7 we
SvS! NOILVLOY 6961
33
8 6 a ub 2 € wt st a ab at at oz te ee & ve se 9 a 82
Ll i 1 a oe r ° ye
vy.
ce
|
% S
=. + Pad |
ees aw |x gaa
i 9
= A x
x
[| (e°9 |
ce SOL S i
CE, De G SK Sane
y 4 y7 * ela 7t Ly
S ane vB PNG ET
— i

09% ore Oe ‘002 oat oot ort ot 001 08 c ov w 0
WSL NOLLVLON 6961

20


SYNOPTIC RADIO MAPS OF THE SUN AT 3.3 mm FOR THE YEARS 1967-1969

by

Earle B. Mayfield and Kennon P. White III
San Fernando Observatory
Space Physics Laboratory

and

Fred I. Shimabukuro
Electronics Research Laboratory

Laboratory Operations
The Aerospace Corporation
El Segundo, California 90245

The Aerospace Corporation millimeter radio telescope was completed in 1963 and has been used
since then for various observations in planetary, solar and stellar research. It is located in
El Segundo, California with coordinates 33° 54' 53" N and +7h 53m 30s (118° 22' 30" W) at a height
of 38m. Since 1966 radio maps of the whole solar disk have been obtained routinely at 90 GHz
(3.3 mm wavelength). An effort has been made to make a map at least once a day, except when con-
ditions of very dense clouds or rain prevail. Consequently, an extensive library of solar data
exists which may be of considerable interest to others

A difficulty in making these observations available is in developing an appropriate format
for publication. The method adopted is based on our investigations of variations of the 3.3 mm
emission and correlations with other solar phenomena which have established relationships with
photospheric magnetic fields, faculae and centers of activity. Further, the regions of enhanced
millimeter emission are well-defined and stable features which can be readily identified and fol-
lowed during disk passage. Transient phenomena associated with flares which have been discussed
by Shimabukuro [1968] are usually at the resolution limit of the antenna and are relatively in-
frequent. As a result, we consider synoptic maps as the most informative presentation and the most
concise. For those who may require more detailed data or individual maps for specific dates, sep-
arate maps can be provided.

Although the instrument has been previously described by Jacobs and King [1965] and by King
et al. [1966], a brief description is appropriate. The antenna is a Cassegrain design of 15-foot
diameter (4.57 meters) in a polar mount. Although the surface has been finished for operation at
400 GHz (1 mm), it is usually operated at 90 GHz (3.3 mm). At this wavelength the beamwidth at the
half-power points is about 2.8 arc-min. Pointing accuracy and stability for the instrument is about
20 arc-sec. The antenna is controlled by an on-line digital computer through a closed loop servo
which permits a variety of tracking modes including a mapping mode which is used for solar studies.
The radiometer is of the Dicke type in which switching is done at 465 Hz between the on-axis beam
and a wide beam sky temperature reference horn. The first stage of the radiometer is a single-
ended gallium arsenide crystal mixer which provides for frequency conversion to a 3 GHz intermediate
amplifier. The system sensitivity for a signal-to-noise ratio of one at the output is about 0.6°K
for 1 second integration time.

For the results reported here, the antenna was programmed to obtain a matrix of emission tem-
peratures centered on the solar disk. A 19x19 matrix was obtained by rastering the antenna between
adjacent points. Four seconds settle time was allowed between readings and one second integration
for temperature measurement. These individual values were normalized to an undisturbed region near
the center of the disk to eliminate the requirement for absolute calibration of the data. This ref-
erence temperature used for normalization was selected by analysis of observations previously obtain-
ed of the mm radio emission together with the Fraunhofer Institut maps to select a quiet region free
of plage or other disturbed emission. One limitation of the maps is that beyond 0.7 R, (normalized
solar radius) the interpretation becomes difficult because of the finite beam width of°the antenna
at the solar limb. As a result, the isotherms are restricted to regions less than 0.7 Rg. Occasion-
al pointing errors also occur in centering the temperature matrix on the disk. These errors are
typically greater than 20 arc-sec but less than 1 arc-min. Occasional variations in cloud cover
can also account for slight differences in the temperature matrix.

A typical map is shown in Figure 1 for 30 June 1971. This has been overlaid on an Ha picture
and isotherms have been constructed on the temperature matrix at levels of 2% enhancement, The
isotherms in Figure 1 indicate the presence of two regions of significant enhancement which can be
identified with the Ha plage in centers of activity associated with magnetic fields in sunspot groups.
The maximum enhancements of these mm regions usually occur near the neutral lines of primary bipolar
magnetic regions and show daily variations associated with the changes in the magnetic fields. Pre-
vious analysis by Mayfield et at. [1970] has discussed these relationships of mm enhancement and
magnetic fields in detail. 1


pop 8 8 8 8 fp ee ef 8 ee ee Te
om
te
lew wae we
+ ees ose)
la
ol-
x x
0 3
oh 29 , x)
Teast r , ao
RAG ovelS es’s ee we
zoP in
oe
o
Ore oz 002 0st oO on oz ol 08 09 oy ra 00
6ES1 NOLLVLOW 2961
Nn
a
aas 43s
@ oe f@ t 2 € » $ 9 £ @ 6 HM H aan so mn aw
oof ye ee ye ee ye ye ee ge ye ee ee
te
| eBin) p+ TL | oe
eue9 \ 99" ( i ))
| x! x4 etd 8% StSe
SS 4 C , a-
wy. ki x x nol
sve }—~ °
| A LY r rf 2a a
ita se" | Ns —_96°5) a2 w
~
ae
| ov
[74 144 002 08 Oo Ort oz 00L 08 09 or oz of

8€S1 NOILVLOW 9961


OSSL NOILVLOY 6961

as 3s
a & we st 9 @ 6 of Loz € ¥ § 9
2 Poot moe oe ee
La
a 9
is’
090 Net A ( Cf?
iz x ]
| _f + Xx = \ i
e's @ SS 91, ¥
6 Cos
OVE OE 08z 002 o8t 09 OF Ott 001 08 09 oF 0 of
1881 NOILVLOW 6961
ony ony
9 8 oe wz @ 6 oO te z ¢€ $ 9 2 6 oO
1° [a i peje ye et cand Poe Let?
~ | eu
— T iC T's 1
Cl le Niet an 2
1 Ty Vy
US rv 2 9 IX xX
x > mi re
‘t vy le
Gy t) ) (daw
3 i
aN Mi Pay
9
Ove 00€ 082 00 08L Om Ov oz OL 08 09 or 0% «of

23


Ne

¥

| |

{

“s.
y
J
ew
rae

4

IN
-

i
Elite.

FSI NOLLVLOY 6961

nue

i)

<0

iC

2yS1 NOILVLOY 8961

19


udv
Z el a aL ot ot ct @ 4 wm Li4 U a €
° ° ce ee oo ° poste
aN
9'8 Tr oF
CAL | Oss
¥ x
|)
= q 2
, °
nN {") ne ed t
. 3 C)
s“s\ es Neve LS Ac
082 02 002 og O9 Ort or cr
S51 NOILVLOY - 8961
udv
uo w zw © Re LB toot ros
fue ues ye je ye ye iP : ae haa
0%] a | | y¢
GY
x v &> £0)
iF) ¥] Ree
DX ro ree be PS x Re
x 7%
Ly aa ENL, er
e v
2 1G), s g : q om
6% \ y mae) V9
—
08z 44 002 oat om orl oF 4

ZeS1 NOLLVLOY - 6961

14


9% [<4 82 62 Of te L 4 £ v s 9 ry 8 6 oO u a eb mn st OL a at él 4 w wz &@
If if 1 ip iP if if i roy of rm
- | -
8 FI ; 4 aio ; : ee
mG Clee: 1-7 eo om DWN | cre Tau -
v) (e% ¥
or X x Ly x x x k 1 ol-
Mod x ra * of a
,
OL = oO
-—— 7 — A m3 — = . oO ¥
w Ss Gre Efe a) aS ~ v ee (423 @} 3 A NER CANCE
— vo 0" 1S f y . ~)
oe S 329 a | Net ae 6 %
b= ra ll eT NS NJ
or o
0096 ‘Ore Ooze 00€ 087 09% Ove Oz 00z 08 om Ort ozt 00L 08 0 or cr4 of
. ‘LIS! NOILVLOU - 1961
©
930 Nve . nue
© wit fz ros 9 2 8 ao ou ua a om = a 4 8 « @ w@ we Re e x
“ee * if i? if if ip yp ip if ip if pop * ff Pp soe oe oe
o- or
oe —_ ray 7 oe
—
we ia 3 | le ey &
&
om x x x4 re o-
ley\ x Ke
eo Ne x oa
o1 we r, ——— 0D) — oO
» RLS (aoa =S== Mies:
é ; :
. SS WN 18 VY NGS Ki) ») (% q Vi NJ «
7 QD, is, =
o o
009E Ore oze 00E 08z 092 we 124 002 OBL O9L Or ozt 0OL 08 09 oF 4 of

SISLNOLLYLOY ~ £961

6961-Z96T SUea, B42 UOJ YIBuaLaAeM uM EE Je UNS aY4Z Jo SdeW OLpey DL3dOUAS

XIGN3dd¥


£9

7.

LN

&

Le

ore

we

orl

9SS1 NOILVLOY 6961

26



“"sqzodsuns pue squauieoueyua

yead usemjeq pue seaue 4e[ndey pue sara] unoqUOD yy ay? usemjaq eouepuodses4o0d 3S019 BY} aJ0N *SaLIULO

PELL!s e432 Aq uMoYS sue SqUeWedUeYUa yeaq ‘sassoud fq pazeOLpul suolfer yainb 243 aroge quaueouRyUa ‘93a 4g

“9 “py $0 S[aAa| 7e B4B SunojUOD sy, ‘apnzLBuoL UeLOS SL B[PIS LCILIUaA *WOPJOG BY 7 UBALB SL gWO 40 a3ep

pue aunBl4 ayq jo doq eyi ye sueadde apnytbuoy Uo}buLuse) *4aLeup_eM Aq auaydsoqoyd ayz yo dew oLydesBot pay
SuLpuodsaiu40d 243 uo pasoduaadns [zg] uolze104 WozBuLuueg 4oj dew snojuoo aunzevsdway oper um ¢*¢ ouqdouks °Z *BL4

wom ow e we we mM @ we wR wR we H HK Loz © > § 5 £ 8 6 wo a
a ee a | a |

MEAEN db RR 5 Fal
m2 ‘ Zn ee Be
as kK o

a}
“3,
a

iv. Iga
2 Dr]
GNSS

(hi

>
XY

.*)
Fe.

is
i
i:
Fan

f

009 Ore oe ‘0 082 097 ore a 002 ot ost ort ot ‘001 08 o %
1251 NOLLVLON - 2961


Fig. 1. The 3.3 mm solar radio temperature contour map made on 30 June 1971 superimposed
on_a concurrent Ha photograph. The contours are jabeled in percent enhancement.
relative to the temperature of the undisturbed region denoted by the hatched con-
tours.

To summarize the results of three years' observation from 1967 through 1969, a synoptic presen-
tation was used based on the Ziirich heliographic maps of the sun by Waldneier [1968] and the magnetic
field presentation of Mt. Wilson by Howard. These maps are arranged to present the 360° of the solar
disk showing the mm isotherms on a day near central meridian passage. A typical synoptic map is
shown in Figure 2 for Carrington rotation 1521. The Carrington longitude is given at the top of the
figure and the date of central meridian passage is located by the filled circle and day number at the
bottom of the figure. The vertical scale is the solar longitude between +#50°. Maps used in the
synoptic presentation have been normalized to the quiet regions indicated by the crosses in the fig-
ure; times at which the maps were obtained are indicated with tic marks at the bottom of the figure.
For presentation in this synoptic format, only isotherms from 4% enhancement up have been used. This
is done to identify enhanced regions and to show the close correlation between the mm enhancement and
white light faculae identified in the Ziirich maps.



nar nar
L t € v s g “ a 6 OL u a el vm st wn a al él ira Ww w@ i4 we s % 4
poy yet pe ye pe ye ye pe ye pe ye ee ee ye ye te tt
o- A or
oe- & i oe
v NN baa ~
5 Tal ¥
- ev &) UW
ov x X x r x be x ov
od eR ra 03
¥. ie ~~
ot 2°S) ve Go oO
¥: q 4 68
. iF. oN @ 5) q ) eat sh) a .
U e°s, Cy iy v
e a *
ov oF
009 OVE 0ze 00€ 08% 09 ove [74 002 08L oot Ort oz OL 08 09 or cr of
SES1 NOLLVLOY - 8961
AY AVA
y s 9 a 8 6 OL tb a eb wm st a at Bl ot 4 w@ 24 &% 4 st 9 le a ee of it
oye ye ef ye © ee ye pe pe pe ye ye eee mo ye ye ee
or or
f
oe oe
Fa: 6°S.
oe Sve 7 —— anh a
i
. ep [¢ aa 4
or ye Xo or
x x oy
Mod > aaa x aed we %& 03
OL fe & io =v. ol
os 94E-§ v v 7 at
w (C9 -) LILES b Me
TM ( 9 / ie "9
ALTAR F we 7
oe 3 7 PA]
ow ov
009 Ove Ooze 00€ 082 09% iz4 02 00z oat 09 ort oz 00L 08 09 oF oz of

VESI NOLLVLOY ~ 8961

15


MAYFIELD, E. B.,
K.P. WHITE III and
F. I. SHIMABUKURO
SHIMABUKURO, F. I.

WALDMEIER, M.

1973

1968
1968

IAU Symposium 57 on Coronal Disturbances, Surfers
Paradise, Australia.

Solar Phys., 5, 498.

Publikationen der Ridgenossischen Sternwarte, Ziirich 13,
Heft 2.



adv AV AWW
ve 4 9 le 8 6z of t z € v s 9 a 8 6 OL ub 2 eb vw st ‘1% ab aL 61 oz
Co oe See eee es ee tt
~~ st) Ly
ets 9
Ly I@ ¥ N\ 2 Ml 5 te 8
rp | So] WO a7 ct a“ a LD
jm. 4+ xu ase FA) I
Pe) kk SNS) | x eof ee’ Ys
— —<
wee —— men J —L-} qd ma
2s °6 18 Bry ( 01
(eee ANIC 3B 112) (Ceo. Noe ew] |, |
| — — bd 8 apna
rs LANs Bay ‘ iO ea
“ 9. Sg —e
268) TN mime.
+ 8 OL
v, y
WEE} |
09E ‘Ove Oze 00€ 08z 09% 4 Oz 002 gL ot Ov zt OL 08 09 ow 4 0
L¥S1 NOILVLOY 6961
Uv udv udv
ee 62 oe te L 2 € v s 9 2 8 6 OL ua a et ob st Ts at el ol oe te zw &
mf oF Ft og of ok 8 8s ote Fe et ot et oe oe oF ee
Ly LL M4
e x — +~p. ED ¥
Le P im Det? CN DOr,
e 0} i's Tt
3 a Ql Sa eA ICP T LES |
q -—T
K 9 '8—19 8: * x a ee x
rN
= wih WRT
oy [97 | &, X t2°9 y
IN AN iG 9) a Us ¢ . Poa
— 2°93 TTM mts
iq ay a\ ca r~Ty 1 Ake y
— St 6
i
009E Ore ‘ze 00€ 08z 09 Ore 07% 002 08t ot ont oz OL 08 09 or 4 of

9¥SL NOLLVLOY 6961

21


WORLD DATA CENTER A
for
Solar-Terrestrial Physics

REPORT UAG-32

SYNOPTIC RADIO MAPS OF THE SUN AT 3.3 mm
FOR THE YEARS 1967-1969

APRIL 1974



i | ff P f i 4 1 14 fof {it f i °
|
YT? LT) _
= Tt iy
a) { 19) ¥ DD Fy an we
L=9' G
DIMER) d x Srl |
-
x} y SA x] x be
3 oa
Ly. aw
ALS] 7 ie en i |
<I @ eeu t ~ GA Val
of; 18 7) eg 3=9 .
Ce HTN 250. J ») ee oie 5 y 9
Ph 1-4-7 N ) I J — N <a]
ov
Ove oe 00E 082 09% Ore Ove 007 oat om orl oz 00 og 09 or ow of
12St NOLLV10¥ ~ 2961
co
AVN AWW
0% ig g g " @ % a 8 & © L z £ v $ 9 L 8 6 a ut a et wm st a
f off i
o-
a Toop SA] oe-
i
(G. Q 0°90 T cepa! sa Dd oF u we
KD) Se" CSS Va e al
a
GaNIv.g0. v 4 GaNIVLEO,
VLVG ON ViVd ON oo 3
crs a
er, 5 0 "
(ee SN Cc mw <n «
Nees | s< )tS an Aas
23 dou Nn =) Las
— ot ss
=. 7 N38 ;
Ore ze 008 082 09% we ez oat om ol ozt 00L 08 09 or 0% 0

ca
0251 NOLLV.LOY - 2961


udv

<4 ir4 a Lr4 4 a % 4 oc ts t € , s 9 r 8 6 OL u a et as st a a at
pote ak ee oe @ «6 7 © © © @
oy be Or
9. N
a ia i, at zoey
- i PANY -
we op 4 — Ro Oy/7 °
MY ie, IN
ol x ol
Hod x x G3NIVLEO VLVG ON: oa
x — V~
et — a
Ne |
v4 oe) a
8.
BOM thers Ny
oe ae
CSU KN =
or or
009E OVE 0ze 00 087 09% Ove [24 002 08 om Ort oz ol 8 09 oF 4 0
6ISI NOLLVLON - 1961
934 uv MW
x4 4 se 54 4 C4 L a € y s 9 r 8 6 oL u a et wm st OL a al 6L v4 i <4
ft i l [et . i | vt if i
o- 7 o-
——s. 29
s p—,
oe vi hey 9°9. = ce-
oO rl | I iF
oe- ee. ‘ CH zt Co = ve (ex P se DL tee oy) a
+ %5 os i G5
oir v" 4 i" ot-
Hod = x Xa
o 1 + | ¥ ey 1
y r~ Me —!
« RS ga he?) AW COA ER ECP MYA A CS.
5 62 | €°6, > ee |
* D) @ aly OL NDI \ as (RS
7 i
be Ns UES iS 4 ;
or ¥ or
009E Ore oe 00€ 082 09% Ove 02 Ort oz 00L 08 09 or 4 00

002 Osi 09
ISL NOILVLOY ~ 1961


UAG-16

UAG-17

UAG-18

UAG-19

UAG-20
UAG-21

UAG-22

UAG-23

UAG-24

UAG-25

UAG-26

UAG-27

UAG-28

UAG-29

UAG-30

UAG-31

"Temporal Development of the Geographical Distribution of Auroral Absorption for 30 Substorm
Events in each of IQSY (1964-65) and IASY (1969)", by F. T. Berkey, V. M. Driatskiy, K.
Henriksen, D. H. Jelly, T. I. Shchuka, A. Theander and J. Yliniemi, September 1971, 131 pages,
price 70 cents.

"TIonospheric Drift Velocity Measurements at Jicamarca, Peru (July 1967-March 1970)", by

Ben B. Balsley, Aeronomy Laboratory, National Oceanic and Atmospheric Administration, Boulder,
Colorado, and Ronald F. Woodman, Jicamarca Radar Observatory, Instituto Geofisico del Perd,
Lima, Peru, October 1971, 45 pages, microfiche only, price 45 cents.

"A Study of Polar Cap and Auroral Zone Magnetic Variations", by K. Kawasaki and S. -I. Akasofu,

Geophysical Institute, University of Alaska, June 1972, 21 pages, price 20 cents.
"Reevaluation of Solar Flares 1967", by Helen W. Dodson and E. Ruth Hedeman, McMath-Hulbert
Observatory, The University of Michigan, and Marta Rovira de Miceli, San Miguel Observatory,
Argentina, June 1972, 15 pages, price 15 cents.

"Catalogue of Data on Solar-Terrestrial Physics", October 1972. (now obsolete).

"Preliminary Compilation of Data for Retrospective World Interval July 26 - August 14, 1972",

compiled by J. Virginia Lincoln and Hope I. Leighton, World Data Center A for Solar-Terrestrial

Physics, November 1972, 128 pages, price 70 cents.

"Auroral Electrojet Magnetic Activity indices (AE) for 1970", by Joe Haskell Allen, National
Geophysical and Solar-Terrestrial Data Center, Environmental Data Service, November 1972,
146 pages, price 75 cents.

"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, U.K., and K. Rawer,

Arie tegruppe fiir Physikalische Weltraumforschung, Freiburg, G.F.R., November 1972, 324 pages,
price $1.75.

"Data on Solar-Geophysical Activity Associated with the Major Ground Level Cosmic Ray Events

of 24 January and 1 September 1971", Parts 1 and 2, compiled by Helen E. Coffey and J. Virginia

Lincoln, World Data Center A for Solar-Terrestrial Physics, December 1972, 462 pages, price
(includes Parts 1 and 2) $2.00.

"Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-41 MHz, 9 September 1968
through 9 December 1971", by James W. Warwick, George A. Dulk and David G. Swann, Department
of Astro-Geophysics, University of Colorado, February 1973, 35 pages, price 35 cents.

"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, May 1973, 129 pages, price 70 cents.

“High Speed Streams in the Solar Wind", by D. S. Intriligator, University of Southern
California, Department of Physics, Los Angeles, California, 90007, June 1973, 16 pages,
price 15 cents.

"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, July 1973, 932 pages,
price (includes Parts 1-3) $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,
Environmental Data Service, October 1973, 148 pages, price 75 cents.

"Catalog of Data on Solar-Terrestrial Physics", prepared by Environmental Data Service,
NOAA, Boulder, Colorado, October 1973, 317 pages, price $1.75.

"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,
Environmental Data Service, February 1974, 142 pages.

USCOMM-NOAA ASHEVILLE, NO=alhn7l}—=1325



G Series of Reports

Prepared by World Data Center A for Solar-Terrestrial Physics, NOAA, Boulder, Colorado, U.S.A.

These reports are for sale through the National Climatic Center, Federal Building, Asheville, NC 28801,
Attn: Publications. Subscription price: $9.00 a year; $2.50 additional for foreign mailing; single
copy price varies. These reports are issued on an irregular basis with 6 to 12 reports being issued
each year. Therefore, in some years the single copy rate will be less than the subscription price,
and in some years the single copy rate will be more than the subscription price. Make check or money
order payable to: Department of Commerce, NOAA.

Some issues are now out of print and are available only on microfiche as indicated. Requests for micro-
fiche should be sent to World Data Center A for Solar-Terrestrial Physics, NOAA, Boulder, Co 80302,
with check or money order made payable to Department of Commerce, NOAA.

UAG-1 "IQSY Night Airglow Data", by L. L. Smith, F. E. Roach and J. M. McKennan of Aeronomy
Laboratory, ESSA Research Laboratories, July 1968, 305 pages, price $1.75.

UAG-2 "A Reevaluation of Solar Flares, 1964-1966", by Helen W. Dodson and E. Ruth Hedeman of
McMath-Hulbert Observatory, The University of Michigan, August 1968, 28 pages, micro-
fiche only, price 45 cents.

UAG-3 "Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-41 MHz, 6 July 1966
through 8 September 1968", by James W. Warwick and George A. Dulk, Department of Astro-
Geophysics, University of Colorado, October 1968, 35 pages, microfiche only, price 45 cents.

UAG-4 “Abbreviated Calendar Record 1966-1967", by J. Virginia Lincoln, Hope I. Leighton and
Dorothy K. Kropp of Aeronomy and Space Data Center, Space Disturbances Laboratory, ESSA
Research Laboratories, January 1969, 170 pages, price $1.25.

UAG-5 "Data on Solar Event of May 23, 1967 and its Geophysical Effects", compiled by J. Virginia
Lincoln, World Data Center A, Upper Atmosphere Geophysics, ESSA, February 1969, 120 pages,
microfiche only, price 90 cents.

UAG-6 "International Geophysical Calendars 1957-1969", by A. H. Shapley and J. Virginia Lincoln,
ESSA Research Laboratories, March 1969, 25 pages, microfiche only, price 45 cents.

UAG-7 "Observations of the Solar Electron Corona: February 1964-January 1968", by Richard T. Hansen,
High Altitude Observatory, Boulder, Colorado and Kamuela, Hawaii, October 1969, 12 pages,
price 15 cents.

UAG-8 "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, March 1970, 312
pages, price (includes Parts 1 and 2) $1.75.

UAG-9 “Data on Cosmic Ray Event of November 18, 1968 and Associated Phenomena", compiled by
J. Virginia Lincoln, World Data Center A, Upper Atmosphere Geophysics, ESSA, April 1970,
109 pages, price 55 cents.

UAG-10 "Atlas of Ionograms", edited by A. H. Shapley, ESSA Research Laboratories, May 1970, 243
pages, price $1.50.

UAG-11 "Catalogue of Data on Solar-Terrestrial Physics", June 1970. (now obsolete).

UAG-12 "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, NOAA, April 1971, 466 pages, price (includes Parts 1-3) $3.00.

UAG-13 "Data on the Solar Proton Event of November 2, 1969 through the Geomagnetic Storm of November
8-10, 1969", compiled by Dale B. Bucknam and J. Virginia Lincoln, World Data Center A, Upper
Atmosphere Geophysics, NOAA, May 1971, 76 pages, microfiche only, price 90 cents.

UAG-14 "An Experimental, Comprehensive Flare Index and Its Derivation for 'Major' Flares, 1955-1969",
compiled by Helen W. Dodson and E. Ruth Hedeman, McMath-Hulbert Observatory, The University
of Michigan, July 1971, 25 pages, price 30 cents.

UAG-15 "Catalogue of Data on Solar-Terrestrial Physics", July 1971. (now obsolete).

|
t
t


Plotted in Figure 2 also is an overlay of sunspots and faculae taken from the Ziirich map for
rotation 1521. This shows a close correlation between the 4% isotherm contour and areas of faculae
in sunspot regions. An interpretation of mm emission and the relation with white light faculae has
been given by Mayfield et al. [1973] and will not be discussed here. Synoptic maps for the years
1967 through 1969 are given in the appendix. These have been plotted so that they can be readily
compared with the Ziirich photoheliographic maps and with the synoptic magnetic field maps published
in the Quarterly Bulletin of Solar Activity.

The question of the longevity of active regions can be investigated by inspection of successive
synoptic maps to note the recurrence of active regions. In this respect it is important to point
out the sensitivity and precision of the data contained in the synoptic maps, because these param-
eters influence the visibility of the enhancements. The lowest contour level plotted corresponds
to_a 4% enhancement, so chosen because at this level individual active regions are usually discern-
able, whereas a 3% contour usually will run nearly the whole length of the map providing very little
information. Additionally, the repeatability of measurements made on different daily maps either on
the same day or different days can be as large as +0.5%, though the average is probably closer to
40.3%, with some outstanding examples showing variations of no more than +0.2% over a five- or six-
day period. To maintain a precision of about 10% (e.g. 4 +0.4%), we felt it was safest to display
the 4% contour as the lowest level.

Therefore, the longevity of an active region is defined as the time from when it first exceeded
4% enhancement to when it first disappeared below the 4% level. Based on this criterion, some regions
are found to last less than a full solar rotation, while others can persist and be followed over five
or six rotations. As will be shown below, this result is entirely consistent with the result that
the 4% contour level coincides in shape and location with the facular areas, which have lifetimes
that can be as short as a few days or as long as a few solar rotations.

Another feature of the synoptic maps whose longevity can be gauged is the quiet regions, as
‘indicated by the clustering of crosses. The nature of these regions is still in question, but
certain examples of them can be followed over three or four rotations.

Daily observations of sunspots and photospheric faculae have been presented in synoptic form
by Waldmeier [1968] in Heliographic Maps of the Photosphere. An example of these maps in Figure 2
shows each sunspot group at the time of its maximum evolution. Umbrae are given as black dots,
penumbrae are shown by their outlines, and facular regions are shown by dashed lines on the maps.

Comparison of the radio synoptic map with the heliographic map in Figure 2 shows how well the
4% enhancement contours correspond to the extensions of the facular regions. Differences in shape
and extent can be attributed to a number of causes, which include: (iy slow, evolutionary changes
in the active regions, since the photospheric maps pertain to the maximum development of the regions,
while the millimeter maps reflect the appearance closest to central meridian passage; (2) rapid
changes in the active regions, as caused by flares, whose residual effects can influence the radio
contours (although, such has been allowed for and corrected when possible); (3) selection of an
invalid normalization point for a particular daily radio map (e.g., a dark absorption filament) ,
which would cause an apparent "growth" or "contraction" of the enhancement levels; and (4) the lack
of a physical connection between the two phenomena.

We hope these results will be of benefit to other investigations of solar phenomena. Subsequent
data will be published as they are reduced and analyzed. Individual maps of particular times, if
available, may be obtained for the years 1970 to the present by communicating with the authors.
Comments or recommendations for improving the format of the presentation are welcomed.

Acknowledgements

This research was supported in part by NASA Ames Research Center under Contract NAS2-7868
and in part by company funds of The Aerospace Corporation.

REFERENCES
JACOBS, E. and 1965 IEEE International Convention Record, Part 5.
H. E. KING
KING, H. E., 1966 IEEE Trans, on Antennas and Propagation, AP-14, 82.
—. JACOBS and
J. M. STACEY
MAYFIELD, E. B., 1970 Solar Phys., 13, 372.
J. HIGMAN and
C. SAMSON



AON
Cr] rr) 7 a] a) a | rn) <<

18

n “4 rif ioe sit ie
or
oe
0z- ze
2% et 'S,
or 4 id
Hoo oF K
x x au x|_ ix
vik

« [Ge a" RN

5 uy Lon cad
oc }28 €°5 LW)
or

oom oe~CSCSC*C“C*‘i SC‘ S*‘“‘ SSCS
IvS1 NOLLVLO¥ 8961
190
si 9) khakis saw € +
ft i 1° A A {__*
or
oe Leb
6% =~ \
* i aA CY SD
a ane Ce
oo x
a x x
x cS
ra TS é ew ‘
% AR Ss ¥
e ae 9's! a
nv 9%
009 Ove oze ‘00E 087 092 Li4 Lc4 002 ost ot orl

OpS1 NOILVLOW 8961


or-
oe-
o>
ot

Mod
ot
w
0

ov

or
oe-
oe-
ol-

Mod
aL
ra
0

ov

190

6

a
st.

=

2

“Ol

EEN
y

ia

tad

;
iS

oe

or

091
ESS1 NOILVLOU 6961

orl

ey

L's:
md

oe

vd

Oe

‘ost

29S1 NOLLVLOY 6961

ort

oz

oo

0

or

oe

a

oi

03

ot

o

o

24




b6"o|
+4

aN _~
ie 4 a
c y's L) } q
C LY Ko
>
|
00€ 0 08L OO or 0
2261 NOLLVLOW - 1961
€ , u a aL mn ir4 4
se 2 8 6 6 oan
c|
x
{aanivigo viva on |} =
MS
00€ 002 08 om

9251 NOLLVLOY - 2961

or

11


YvW yw
5A AT TS A L z £ , s 9 Log 6 OL
¢ je © © © | © 9 © 6 © wo 0 © © »© © € § ee ~@ 6 2 8 10 Je

| 1 | | yp of on I 1°?
o-
oe + Va a \ |_|.
oe rel 3h los \ foinl | @., ( (Fe) JS fam a eed y
g ° TM XI 4 94 ie" Ny,
a Lt NY | (as wo}? LJ °F, Ss) 7 we
ee x i " q Le x
od x4 x x
oO (= s ont. v7 mee v4
‘ 5
RS Ur TT Sie (Sel ea | i
we ff “e—
3) pe" Li (2 3 ¢ s
of zy Las
7
009E Ove 0ze 00 082 092 Ove 4 002 oat ool OFL oz 00L 08 09 or 4 0
I€SL NOLLVLOY - 6961
Nur 934 934
oo ae BL él % 3 az &@ " St % a & 4 0 ie t g € s 9 é 8 6 oO ut a
. fo ! 1° | ! | io yor ye
o- = ra
_ L—- Lv¥@)
~ £9 —>
ey 10] ) gee vi~A
oe~ ® 7 8 4 , 9
; \ e— (e Ly "op Gs) ms p+ ap)
* x —T x Ltr x x hk oy yi
Mod
we |_—
o 7 s)) ( = ny votes. _
Foxes vt 9. LRN s 5s Nw
@ ts: 7 Ime
Ly Gi ° 2e'9 bt er C ee) I} (ere (F jon
o ° le “ou wai
5 Se
TN —
o |
009 Ove Oe 00E 08z 09 Ore 02 00 oat ot Ort oz OL og 0 oF 4 0

O€S1 NOILV.LOY - 8961

13


WORLD DATA CENTER A

for
Solar-Terrestrial Physics

REPORT UAG-32

SYNOPTIC RADIO MAPS OF THE SUN AT 3.3mm
FOR THE YEARS 1967-1969

by
Earle B. Mayfield and Kennon P. White III

San Fernando Observatory
Space Physics Laboratory

and

Fred I. Shimabukuro

Electronics Research Laboratory

Laboratory Operations
The Aerospace Corporation Mi)
El Segundo, California 90245
Prepared by World Data Center A for i)

Solar-Terrestrial Physics, NOAA, Boulder, Colorado
and published by

U.S. DEPARTMENT OF COMMERCE
NATIONAL OCEANIC AND ATMOSPHERIC ADMINISTRATION

ENVIRONMENTAL DATA SERVICE
Asheville, North Carolina, USA 28801

APRIL 1974

SUBSCRIPTION PRICE: $9.00 a year; $2.50 additional for foreign mailing; single copy price
varies.* Checks and money orders should be made payable to the Department of Commerce, NOAA.
Remittance and correspondence regarding subscriptions should be sent to the National Climatic
Center, Federal Building, Asheville, NC 28801, Attn: Publications.

“Price of this issue 35 cents



or

oe-

oe-

or

Mod

ot

o

oe

o

oe x4 6e Of L z € a el oh
eit | oe ° vet
eu
an "
NT
~y— x ro) } +]
x s fd
69 yr
L's:
od IN
A . ie:
Cla M14
s9 9
——
Ove 002 aL OL Ov or oe 0
6¥S1 NOILVLOY 6961
nar nar
oz 0 z € b § 9 woosk kot
cari moe Gani 5
—
2 2s 14 J
¥ oF x
a Z =p
s) ( g 5
LAY
<A Ss ap)
v SR
we oon ori oF Cre)

BbSL NOILVLOY 6961

w-

ol-

0 3

aL
4

or

22


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 eight 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

Solar and Interplanetary Phenomena,
Ionospheric Phenomena, Flare-Associated

Events, Geomagnetic Variations, Magnetospheric

and Interplanetary Magnetic Phenomena,
Aurora, Cosmic Rays, Airglow:
World Data Center A
for Solar-Terrestrial Physics
National Oceanic and Atmospheric
Administration
Boulder, Colorado, U.S.A. 80302
Telephone (303) 499-1000 Ext. 6467

Geomagnetism, Seismology, Gravity (and
Upper Mantle Project Archives) :
World Data Center A:
Geomagnetism, Seismology and Gravity
Environmental Data Service, NOAA
Boulder, Colorado, U.S.A. 80302
Telephone (303) 499-1000 Ext. 6311

Glaciology:
World Data Center A:
Glaciology
U.S. Geological Survey
1305 Tacoma Avenue South
Tacoma, Washington, U.S.A. 98402
Telephone (206) 593-6502

Longitude and Latitude:
World Data Center A:
Longitude and Latitude
U. S. Naval Observatory
Washington, D. C., U.S.A. 20390
Telephone (202) 254-4547

Notes:

Meteorology (and Nuclear Radiation):
World Data Center A:
Meteorology
National Climatic Center
Federal Building
Asheville, North Carolina, U.S.A.
28801
Telephone (704) 254-0683

Oceanography:
World Data Center A:
Oceanography
National Oceanic and
Atmospheric Administratioh
Rockville, Maryland, U.S.A. 20852
Telephone (202) 426-9052

Rockets and Satellites:
World Data Center A:
Rockets and Satellites
Goddard Space Flight Center
Code 601
Greenbelt, Maryland, U.S.A. 20771
Telephone (301) 982-6695

Tsunami:
World Data Center A:
Tsunami
National Oceanic and Atmospheric
Administration
2525 Korrea Road
Honolulu, Hawaii, U.S.A. 96822
Telephone (808) 948-8083

(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.



‘AON 030 03a
es oe oF FL 2 € vv S$ 9 L 8 6 OL Lh a E + SE O at ot 6 o2 te 2 e€ v2

\

a.

<P

009

er

002 ogi oot
SSSI NOILVLOY 6961

a

7

se

9

a

cy,

Sp

6

S’y

0096 One

oe

(008

087

0%

ove

we

007 ogi ost
S51 NOLLVLOY 6961

‘ort

ot

oot

o

25


ant ony ony
6 a Ww au & om ss 8 4 & & & wk wz we wR & ww 2 ew w@ © ww 1 ct © r ¢
or ep ae eae eee Taal oof ye fF yee ee
L -
+
pr m of-
> ; or °
i = seta cS :
Ty oe Se <5 we
i, ~ amd h Le
x % 4 ol-
30d
02
x,
Ax x be ~ 4
LT [AL Gta Oo
is aft a y z
* Lr.
C SEP @ l #85 oe
Se e x
o
009% Ove oe 0E 08z 09% Oe 02 002 OBL ot Ori ozt 00L 08 09 OF [v4 0
€ZSLNOILYLON - £961
nar nr ane
a et wm st a a a ot V4 w cc4 4 % 4 w a 4 C4 of L a € , s 9 “ 8 6
ie Oe a | * Pr pee foe Pr ie Ff 1°
Or
oe
y &s
& ) A fash (os 2 |’ yy ys. e Us. Ct,
rs @ Loy ae e i we
Lr wy ok, NJ Uy , +7 ie)
x Wx ol-
x
Eg ¥ a x 3
OL
= ~X >
Lott NN om Th TM G qe e
- OP tO tao a, (Oe <eie
iP % = 9
——) No J NI 50 «
ov
09 Ore oe 00E 08z 09% ve Oz 007 ost Oo Ov ozt 00L 08 0 ow [r4 0

ZSLNOLLVLON — £961


O30
Zz

or

or

\(

oa-

\*

a

wd

o1-

re x

Hod

OL

rv

a)
A]

K
J
U7

oo

a

oe

ow

082

002 08 091
6281 NOILVLON - 9961

oz

ou

or

93a
a 6L

x!

a)

ove

WE

09%

ore

oz

002 ‘081 o9t
82S1 NOILVLOY - 1961

ort

ca

01

08

12