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20


SYNOPTIC RADIO MAPS OF THE SUN AT 3.3 mm, 1970-1973
by

Earle B. Mayfield
Space Sciences Laboratory

and

Fred I, Shimabukuro
Electronics Research Laboratory

The Ivan A, Getting Laboratories
The Aerospace Corporation
E1 Segundo, California 90245

INTRODUCTION

The Aerospace Corporation millimeter radio telescope, which was completed in 1963, has been used
extensively for investigations in planetary, solar, and stellar research. It is located in El] Segundo,
California, at 30°54'53"N and 118°22'30"W (7h 53m 30s) at a height of 38 m. Maps of the whole solar
disk at 90 GHz (3.3-mm wavelength) were obtained routinely on a near daily basis from 1966 through
1973, In October 1973, loss of funding resulted in the discontinuation of the solar program. Since
then, only infrequent observations of the Sun have been made to calibrate the radiometer.

The format used in presenting millimeter radio observations is the same as that employed for pre-
vious results [Mayfield et al., 1974] and is based on investigations of variations in the 3.3-mm emission
and its correlation with photospheric magnetic fields, faculae, and centers of activity. Furthermore,
the regions of enhanced millimeter emission are well-defined, stable features that can be readily identi-
fied and followed during their disk passage. The relatively infrequent, transient phenomena associated
with flares, which have been discussed by Shimabukuro [1968], usually lie at the resolution limit of
the antenna. As a result, synoptic maps are considered not only the most informative presentation but
the most concise. The authors can provide separate maps for those individuals who require more detailed
data or individual maps for specific days.

INSTRUMENT DESCRIPTION

The polar-mounted antenna is Cassegrain in design and 4.57 m (15 ft) in diameter [Jacobs and King,
1965; King et al., 1966]. Although the surface has been finished for operation at 400 GHz (1 mn), 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. An on-line
digital computer controls the antenna through a closed loop servo that permits a variety of tracking
modes, including a mapping mode for solar studies. The radiometer is of the Dicke type in which switch-
ing 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-end gallium arsenide crystal mixer that provides for frequency con~
version to a 3-GHz intermediate amplifier. The system sensitivity for a signal-to-noise ratio of 1 at
the output is about 0.6 K for a 1-second integration time.

For the results reported here, the computer-controlled antenna was programmed to obtain a square
array of emission temperatures centered on the solar disk. A 19 x 19 matrix was obtained by rastering
the antenna between adjacent points. A 4-second settle time was allowed between readings with a 1-sec-
ond integration time for temperature measurement. These individual values were normalized to an undis-
turbed region near the center of the disk to eliminate the requirement of absolute data calibration.
This reference temperature used for normalization was selected by analyzing millimeter observations
previously obtained and by using the Fraunhofer Institute maps to select a quiet region free of plage
or other disturbed emission. The finite beamwidth of the antenna at the solar limb restricts interpreta-
tion and thus the isotherms to regions less than 0.7Rg (normalized solar radius). The maps contain this
limitation. Others include occasional pointing errors, typically greater than 20 arc-sec but less than
1 arc-min, that occur in centering the temperature matrix on the disk and slight differences in the
emission temperatures owing to variations in cloud cover.

Figure 1 shows a typical map dated 30 June 1971 that has been superposed on an Ha picture. Isotherms
have been constructed on the temperature matrix at levels of 2% enhancement, and they indicate in this
case the presence of two regions of significant enhancement--ones that can be identified with Ha plage
in centers of activity associated with spot group magnetic fields. The maximum enhancement in these
millimeter regions usually occurs near the neutral line of a primary bipolar magnetic feature and shows
daily variations associated with changes in the magnetic fields. In a previous analysis, Mayfield et
al. [1970] have discussed in detail the relation between millimeter enhancement and magnetic fields.

1



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"Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-80 "Hz 10 December 1971 through 21 March 1975",
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“Catalog of Observation Times of Ground-Based Skylab-Coordinated Solar Observing Programs", compiled by Helen E.
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"Synoptic Maps of Solar 9.1 cm Microwave Emission from June 1962 to.August 1973", by Werner Graf and Ronald N.
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"Auroral Electrojet Magnetic Activity Indices AE (11) for 1972", by Joe Haskell Allen, Carl C, Abston and Leslie
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"Interplanetary Magnetic Field Data 1963-1974", by Joseph H, King, National Space Science Data Center, NASA Goddard
Space Flight Center, Greenbelt, Maryland 20771, June 1975, 382 pages, price $2.95.

“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, Environmental Data Service, June 1975,
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490

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“synoptic Observations of the Solar Corona during Carrington Rotations 1580-1596 (11 October 1971 - 15 January 1973)";
(Reissue with quality images] by R. A. Howard, M. J. Koomen, D, J. Michels, R. Tousey, C, R, Detwiler, D. E,
Roberts, R. T. Seal and J. D. Whitney, E. 0. Hulbert Center for Space Research, NRL, Washington, D. C. 20375
and R. T. and S. F. Hansen, C. J. Garcia and E. Yasukawa, High Altitude Observatory, NCAR, Boulder, Colorado
80303, February 1976, 200 pages, price $4.27.

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

“High-Latitude Supplement to the URSI Handbook on Ionogram Interpretation and Reduction", by W. R. Piggott, British
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"Synoptic Maps of Solar Coronal Hole Boundaries Derived from He II 304 Spectroheliograms from the Manned Skylab
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“Experimental Comprehensive Solar Flare Indices for Certain Flares, 1970-1974", compiled by Helen W. Dodson and
E. Ruth Hedeman, McMath-Hulbert Observatory, The University of Michigan, 895 Lake Angelus Road North, Pontiac,
Michigan 48055 U.S.A., November 1975, 27 pages, price 60 cents.

"Description and Catalog of onospheric F-Region Data, Jicamarca Radar Observatory (November 1966 - April 1969)", by
WoL. Clark and T. E. Van Zandt, Aeronomy Laboratory, NOAA, Boulder, Colorado 80302 and J. P. McClure, University
of Texas at Dallas, Dallas, Texas 75230, April 1976, 10 pages, price 33 cents,

“Catalog of Ionosphere Vertical Soundings Data", prepared by Environmental Data Service, NOAA, Boulder, Colorado
80302, April 1976, 130 pages, price $2.10.

“Equivalent Ionospheric Current Representations by a New Method, Illustrated for 8-9 November 1969 Magnetic Disturb-
ances", by Y. Kamide, Cooperative Institute for Research in Environmental Sciences, University of Colorado,
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Data Studies Division, NOAA/EDS/NGSDC, Boulder, Colorado 80302, M. Kanamitsu, Advanced Study Program, National
Center for Atmospheric Research, Boulder, Colorado 80303, J. H. Allen, Data Studies Division, NOAA/EDS/NGSDC,
Boulder, Colorado 80302, and S.-I. Akasofu, Geophysical Institute, University of Alaska, Fairbanks, Alaska
99701, April 1976, 91 pages, price $1.60.

“Iso-intensity Contours of Ground Magnetic H Perturbations for the December 16-18, 1971 Geomagnetic Storm", by
Y. Kamide, Cooperative Institute for Research in Environmental Sciences, University of Colorado, Boulder,
Colorado 80302 and Geophysical Institute, University of Alaska, Fairbanks, Alaska 99701 (currently Guest worker
at Data Studies Division, NOAA/EDS/NGSDC, Boulder, Colorado 80302), April 1976, 37 pages, price $1.39.

“Manual on Ionospheric Absorption Measurements", edited by K. Rawer, Institut flir Physikalische Weltraumforschung,
Freiburg, G.F.R., June 1976, 202 pages, price $4.27.

"ATS6 Radio Beacon Electron Content Measurements at Boulder, July 1974 - May 1975", by R. B. Fritz, Space Environment
Laboratory (currently with Wave Propagation Laboratory), NOAA, Boulder, Colorado 80302 USA, September 1976,
61 pages, price $1.04.

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

"Geomagnetic Data for January 1976 (AE(7) Indices and Stacked Magnetograms)" by J. H. Allen, C. A. Abston and
L. R. Morris, NGSDC/EDS/NOAA, July 1977, 57 pages, price $1.07.

“Collected Data Reports for STIP Interval II 20 March - 5 May 1976", edited by Helen E. Coffey and John A.
Hekinnon, National Geophysical and Solar-Terrestrial Data Center, Environmental Data Service, August 1977,
313 pages, price $2.95.

“Geomagnetic Data for February 1976 (AE(7) Indices and Stacked Magnetograms)" by J. H. Allen, C. A. Abston and
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“Geomagnetic Data for March 1976 (AE(7) Indices and Stacked Magnetograms)" by J. H. Allen, C. A. Abston and
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"Geomagnetic Data for April 1976 (AE(8) Indices and Stacked Magnetoc rams)" by J. H. AT
L. R. Morris, NGSDC/EDS/NOAA, February 1978. uetograns)" by J. de ATTans C. A. Abston end

‘USCOMM-NOAA-ASHEVILLE ,NCS/78~-950



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Figure 1. The 3.3-mm solar radio temperature contour map made on 30-June 1971
superposed on a concurrent Hx photograph. The contours are labeled
in percent enhancement relative to the temperature of the undisturbed
regions denoted by the hatched contours.

SUMMARY OF RESULTS

During the 4 years of observations (from 1970 through 1973) a synoptic presentation was used based
on the Ziirich heliographic maps of the Sun by Waldmeier [1968] and on the magnetic field presentation
of Mt. Wilson by Howard. These maps are arranged to present the 360° of solar longitude, showing the
millimeter 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. Solar
latitude between #50° forms the vertical scale. Maps used in the synoptic presentation have been nor-
malized to the quiet regions indicated by the crosses in the figure; times at which the maps were obtain-
ed are indicated with tic marks at the bottom of the figure. For presentation in this synoptic format,
only isotherms representing 4% or more enhancement have been used, because they identify enhanced re-
gions and show the close correlation between the millimeter enhancement and white light faculae evident
in the Ziirich maps.

Also plotted in Figure 2 is an overlay of sunspots and faculae taken from the Ztirich map for rota-
tion 1521. This shows a close correlation between the 4% isotherm contour and areas of faculae in sun-
spot regions. An interpretation of millimeter emission and its relation to white light faculae has
been given: by Mayfield et al. [1973] and will not be discussed here. Synoptic maps for 1970 through
1973 are given in the appendix.

Synoptic maps for 1970 through 1973 are given in the appendix. They have been plotted to facili-
tate comparison with the Zurich photoheliographic maps and with the synoptic magnetic field maps pub-
lished. in the IAU's Quarterly Bulletin of Solar Activity.

2



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Synoptic Radio Maps of the Sun at 3.3 mm, 1970-73



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Upper Atmosphere Geophysics

REPORT UAG-66

SYNOPTIC RADIO MAPS OF THE SUN AT 3.3mm
1970-1973

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The longevity of active regions can be investigated by inspecting successive synoptic maps and
noting 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 parameters influence the visi-
bility of the enhancements, The lowest contour level plotted corresponds to a 4% enhancement, so chosen
because individual active regions at this level are usually discernible. A 3% contour, on the other
hand, typically runs nearly the length of the map, providing very little information. Additionally,
measurements made on different daily maps, either on the same day or on different days, can vary as
much as +0.5%. The average, though, probably lies closer to +0.3%; some outstanding examples show vari-
ations of no more than +0.2% over a 5- or 6-day period. To maintain a precision of about 10% (e.g.

4 +0.4%), it was safest to display the 4% contour as the lowest level.

Therefore, the longevity of an active region is defined as the time it first exceeds the 4% en-
hancement level to the time it first drops below that level. Based on this criterion, some regions are
found to last less than a full solar rotation; others can persist and be followed over 5 or 6 rotations.
As will be shown below, this result is entirely consistent with the strong correlation between the
shapes and locations of the 4% contour levels and the outlines of the facular areas--areas that can
have lifetimes as short as a few days or as long as a few solar rotations.

As indicated by the clustering of crosses, quiet regions represent another feature of the synoptic
maps, the longevity of which can be gauged. Certain examples of these regions can be followed over 3
or 4 rotations even though their nature remains in question.

Daily observations of sunspots and photospheric faculae have been presented in synoptic form by
Waldmeier [1968] in Heliographie Maps of the Photosphere. An example of these maps (Figure 2) shows
each sunspot group at the time of its maximum evolution. In the maps umbrae are depicted by black dots,
penumbrae by their outlines, and faculae by dashed lines.

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 that include (1) slow, evolutionary changes in the active
regions occurring between the maximum phase captured in the photospheric maps and the stage nearest
central meridian passage reflected in the millimeter maps; (2) flare-induced rapid changes in the active
regions, the residual effects of which can influence the radio contours (although, such effects have
been allowed for and corrected whenever possible); (3) selection of an invalid normalization point for
a particular daily radio map such as a point containing a dark absorption filament, which would cause
an apparent "growth" or "contraction" of the enhancement levels; and (4) lack of a physical connection
between the millimeter emission and the white light faculae and sunspots.

ACKNOWLEDGMENTS
This research was supported in part by company funds of The Aerospace Corporation
REFERENCES
JACOBS, E. and 1965 "2.8 minute beamwidth, millimeter-wave antenna
HoE. KING measurement and evaluation," I&EE International
Convention Record, Part 5, 92-100.
KING, HoE., 1966 "A 2.8 arc-min beamwidth antenna: lunar eclipse
E. JACOBS and observations at 3.2 mm," IEEE Trans. on Antennas
J.M. STACEY and Propagation, AP-14, 82-91.
MAYFIELD, E.B., 1970 "Variations in solar emission at 3.3 mm wavelength
J. HIGMAN and and their relation to flares," Solar Phys., 13
C. SAMSON 372-388.
MAYFIELD, E.B., 1973 "Millimeter radio evidence for containment
K.P. WHITE III and mechanisms in solar flares," in Coronal Disturbances,
FI. SHIMABUKURO TAU Symposium 57, Gorden Newkirk, Jr., Ed. (D. Riedel
Publishing Company, Dordrecht), 447-460.
MAYFIELD, E.B.; 1974 "Synoptic radio maps of the sun at 3.3 mm for the
K.P. WHITE III and years 1967-1969," Report UAG-32, (Department of
F.1. SHIMABUKURO Commerce, NOAA/NGSDC, Boulder, CO)
SHIMABUKURO, F.I. "1968 "A comparison of 3.3-mm bursts and Ha emission during

flares," Solar Phys., 5, 498-506.

WALDMEIER, M. 1968 "Heliographic maps of the photosphere for the year
1967," Publikationen der Eidgendssischen Sternwarte
Biinich, 13, No. 2.

4

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13


WORLD DATA CENTER A
for
Solar-Terrestrial Physics

REPORT UAG-66

SYNOPTIC RADIO MAPS OF THE SUN AT 3.3mm
1970-1973

by
Earle B. Mayfield

Space Sciences Laboratory

and

Fred I. Shimabukuro

Electronics Research Laboratory

The Ivan A. Getting Laboratories
The Aerospace Corporation
El Segundo, California, USA 90245

May 1978

Published by World Data Center A for Sy
&

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

3, %
U.S. DEPARTMENT OF COMMERCE SS
NATIONAL OCEANIC AND ATMOSPHERIC ADMINISTRATION Aw
ENVIRONMENTAL DATA SERVICE
Asheville, North Carolina, USA 28801

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 .75 CENTS



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

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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.



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