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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 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, Meteorology (and Nuclear Radiation):

Ionospheric Phenomena, Flare-Associated World Data Center A:
Events, Geomagnetic Variations, Magnetospheric Meteorology
and Interplanetary Magnetic Phenomena, National Climatic Center

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:

Federal Building

Asheville, North Carolina, U.S.A.
28801

Telephone (704) 254-0683

Oceanography:
World Data Center A:
Oceanography
National Oceanic and
Atmospheric Administration
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.



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2.4 HF Doppler Observations at NASA Marshall Space Flight Center

Figure 2.4 illustrates the HF Doppler experiment at NASA Marshall Space Flight Center near
Huntsville, Alabama, which was designed to study moving ionospheric irregularities including travel-
‘ing waves excited by static ground tests of large rocket engines. The experiment is similar to that
at the University of Leicester, but includes more frequencies to obtain information on the varia-
tions with height. Observations for several flares observed by the ATM-SKYLAB experiments during
the second and third manned missions were studied. Ionograms were not available for this locality

for these events, so the preflare ionosphere was estimated from ionospheric conditions at similar
latitudes and local times.

2.5 HF Doppler Observations in Hawaii

HF Doppler measurements are made by the Radio Science Laboratory of the University of Hawaii at
the field stations shown in Figure 2.5, under Grant Number GA-23964 of the National Science Foundation,
to observe SFDs, various types of traveling ionospheric disturbances, and other time variations of
the ionosphere. SFDs are routinely detected, scaled, and then reported in Solar-Geophysical Data.
Tonograms recorded at Maui, Hawaii, were used to determine the preflare ionosphere electron density
as a function of height. SFDs observed in Hawaii were used to confirm the detailed time structure
of many of the SFDs observed near Boulder, and were the sole source of data for many flares observed
by ATM-SKYLAB, especially during the 0000 to 0400 UT period.


AN ATLAS OF EXTREME ULTRAVIOLET FLASHES OF SOLAR FLARES OBSERVED VIA SUDDEN
FREQUENCY DEVIATIONS DURING THE ATM-SKYLAB MISSIONS if

by

R. F. Donnelly’, E. L. Berger, Lt. J. D. Busman?,
B. Henson*, T, B. Jones*, G. M. Lerfald®, K. Najita®, |

W. M. Retallack?, and W. J. Wagner?

ABSTRACT

The 10-1030A impulsive solar flux enhancements of solar flares during f
the ATM-SKYLAB missions are presented. The extreme-ultraviolet (EUV) en- '
hancements were observed via sudden frequency deviations (SFD), an iono-
spheric effect caused by the enhancement of ionospheric photoionization
produced by EUV bursts. The SFD measurements were made at Sacramento Peak
Observatory; Boulder, Colorado; Leicester, England; Huntsville, Alabama;
and Hawaii. EUV bursts are reported for the period April 1, 1973 to
February 8, 1974, which includes several solar rotations before the first
manned mission of ATM-SKYLAB. Compared to SFD observations from September,
1960 to July, 1970, the ATM-SKYLAB missions were periods of low solar
activity when no large SFDs occurred. However, several medium sized events
did occur with quasi-periodic or extensive fine time structure

1. INTRODUCTION

A sudden frequency deviation (SFD) is a rapid change in the received frequency of a high-
frequency radio wave propagated from an ultrastable transmitter and reflected at altitudes in the
range 120 to 300 km in the ionosphere. This particular type of frequency deviation results from the
time-varying ionospheric electron density produced by the time-varying ionizing radiation from a
solar flare. In effect, SFD observations are like those from a broadband satellite detector, except
SFDs are particularly sensitive to impulsive 10-1030A bursts and relatively insensitive to gradual
rise and fall events [Donnelly, 1970]. SFDs have fairly good time resolution, namely several seconds
for some of the measurements discussed later. SFDs supplement the excellent ATM-SKYLAB observations,
which have high spatial and spectral resolution, by providing high time resolution measurements of
the impulsive flare emissions originating from source regions that are like the chromosphere and
chromosphere-corona transition region, and by providing background information on the occurrence of
EUV bursts at times or spatial locations unobserved by the ATM experiments.

ATM-SKYLAB observations [Reeves, 1972] are the best soft x-ray and EUV observations of the sun |
made to date, because of their high spatial resolution and long duration and because measurements
were simultaneously recorded at many wavelengths. The ATM (Apollo Telescope Mount) measurements of
the quiet sun, solar prominences and active regions are excellent, and should lead to major advances
in understanding their physical properties and processes. The ATM solar observations covered the
period May 29 through June 18, 1973, during the first manned mission of SKYLAB; the period August 7
through September 21, 1973, during the second manned mission; and the period November 26, 1973
through February 3, 1974, during the final manned mission. The Harvard EUV experiment operated also
during the interim unmanned periods. This atlas of SFD observations presents the events in chronological
order in six time periods as shown in Figure 1.1, namely: (1) before the ATM observations, (2)
during the first manned ATM observing period, (3) the first unmanned ATM observing period, (4) the
second mannned ATM observing period, (5) the second unmanned ATM observing period, and (6) the third
manned ATM observing period.

|
|

Author Affiliation:

1. NOAA Space Environment Laboratory, Boulder, Colorado 80302 USA

2. NOAA Commissioned Corps, Boulder, Colorado 80302 USA

3. NASA Marshall Space Flight Center, Alabama 35812 USA

4, Department of Physics, University of Leicester, Leicester, England, UK

5. NOAA Wave Propagation Laboratory, Boulder, Colorado 80302 USA

6. Radio Science Laboratory, Department of Electrical Engineering, University of Hawaii, ij
Honolulu, Hawaii 96822 USA |

7. Sacramento Peak Observatory, AFCRL, Sunspot, New Mexico 88349 USA

1



5. OBSERVATIONS DURING THE FIRST MANNED MISSION OF ATM-SKYLAB

The first manned ATM observations during SKYLAB II covered the period May 29 to June 18, 1973. if
The SFD observing times during the first manned ATM mission are illustrated in Figures 5.1 and 5.2
for the Sacramento Peak and Boulder HF Doppler observations respectively. The Boulder observations
included at least one high sensitivity path reflected from the F-region 96% of the time. The level
of solar activity was quite low during this three-week period; the daily average 10 cm flux measured
at ARO, Ottawa, was below 100 the entire period. Few SFDs were observed. Their main features are
listed in Table 5.1. The two events where the SFD was large enough and the data of sufficient
quality were analyzed to estimate A®(10-1030A, t); the main results are presented in Table 5.2.

WWV Sacramento Peak Observatory
HF Doppler Observations

X= 90° 80°

a ee

anne nee ee ee ee
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T
1400

Figure 5.1 SFD observing time at Sacramento Peak Observatory
during the first manned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

Boulder HF Doppler Observations

k
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+++ No F-region observations

Figure 5.2 SD observing time near Boulder, Colorado during
the first manned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

42 |



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- 36

REPORT UAG

WORLD DATA CENTER A
for
Solar-Terrestrial Physics

AN ATLAS OF
EXTREME ULTRAVIOLET FLASHES
OF SOLAR FLARES OBSERVED
VIA SUDDEN FREQUENCY DEVIATIONS
DURING THE ATM-SKYLAB MISSIONS

Yu

OCTOBER 1974



TABLE OF CONTENTS

ABSTRACT
1. INTRODUCTION
2. HF DOPPLER OBSERVATIONS

At Sacramento Peak Observatory

Near Boulder, Colorado

In England

At NASA Marshall Space Flight Center
In Hawaii

NYNNYND
GRORL

SFD ANALYSIS PROCEDURES

OBSERVATIONS DURING TWO SOLAR ROTATIONS BEFORE THE ATM-SKYLAB
OBSERVATIONS DURING THE FIRST MANNED MISSION OF ATM-SKYLAB
OBSERVATIONS DURING THE FIRST UNMANNED MISSION OF ATM-SKYLAB
OBSERVATIONS DURING THE SECOND MANNED MISSION OF ATM-SKYLAB
OBSERVATIONS DURING THE SECOND UNMANNED MISSION OF ATM-SKYLAB
OBSERVATIONS DURING THE THIRD MANNED MISSION OF ATM-SKYLAB
DISCUSSION

ACKNOWLEDGEMENTS

REFERENCES

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9. OBSERVATIONS DURING THE THIRD MANNED MISSION OF ATM-SKYLAB

The third and last manned ATM observations (SKYLAB IV) spanned the time from about 1900 UT
November 26, 1973, to February 3, 1974, for the photographic recordings. The level of solar activity
was low. The daily average 10 cm radio flux was below 100 radio flux units during this entire
mission and dipped below 80 to nearly sunspot minimum values during the periods December 4 to 16, 1973;
December 29, 1973, to January 9, 1974; and January 24 to the end of the mission. Relatively few flares
occurred that were large enough to cause detectable terrestrial effects. The short daily observing
period at northern latitudes further reduced the number of SFDs detected at Sacramento Peak and
Boulder. See Figures 9.1 and 9.2. The detected SFDs are listed in Table 9.1 and the computed
10-1030A flux enhancement in Table 9.2. Many of the SFDs detected during this period were observed
at the University of Hawaii, where the daily observing period was significantly longer than at the
other observatories and the mid-day solar zenith angle significantly smaller.

The Boulder and Sacramento Peak data were poor in quality for most of these flares. Consequently,
the EUV flux enhancement was computed only for the flare of 2334 UT December 23, 1973, shown in
Figures 9.3 and 9.4, which was well observed in Hawaii.

WWV Sacramento Peak Observatory
HF Doppler Observations

5 X=90° 80° 80° 90°
2 a a et PO a es es es ee i dl 1
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T TMT
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TT TT
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‘No sunit observations
++ No Frregion observations

Figure 9.1 SFD observing time at Sacramento Peak Observatory
during the third manned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

89

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T

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Figure 4.1 SFD observing time at Sacramento Peak Observatory
during two solar rotations prior to the ATM observations.

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12

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54


UAG 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
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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-
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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-
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UAG-3 "Observations of Jupiter's Sporadic Radio Emission in the Range 7.6-41 MHz, 6 July 1966
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UAG-4 "Abbreviated: Calendar Record 1966-1967", by J. Virginia Lincoln, Hope I. Leighton and
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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,
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UAG-6 "International Geophysical Calendars 1957-1969", by A. H. Shapley and J. Virginia Lincoln,
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UAG-10 "Atlas of Ionograms", edited by A. H. Shapley, ESSA Research Laboratories, May 1970, 243
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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",
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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
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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)



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WORLD DATA CENTER A
for
Solar-Terrestrial Physics

REPORT UAG - 36

AN ATLAS OF EXTREME ULTRAVIOLET FLASHES OF
SOLAR FLARES OBSERVED VIA SUDDEN FREQUENCY

DEVIATIONS DURING THE ATM-SKYLAB MISSIONS

by
R.F. Donnelly: E.L. Berger; Lt. J.D. Busman’® B. Henson® T.B. Jones*
G.M. Lerfald® K. Najita’ W.M. Retallack’ and W.J. Wagner’

Author Affiliation:
1. NOAA Space Environment Laboratory, Boulder, Colorado 80302 USA

2. NOAA Commissioned Corps, Boulder, Colorado 80302 USA

3. NASA Marshall Space Flight Center, Alabama 35812 USA

4. Department of Physics, University of Leicester, Leicester, England, UK

5. NOAA Wave Propagation Laboratory, Boulder, Colorado 80302 USA

6. Radio Science Laboratory, Department of Electrical Engineering,
University of Hawaii, Honolulu, Hawaii 96822 USA

7. Sacramento Peak Observatory, AFCRL, Sunspot, New Mexico 88349 USA

OCTOBER 1974

Sy

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

U.S. DEPARTMENT OF COMMERCE =
NATIONAL OCEANIC. AND ATHOSPHERIC ADINTSTRATION TIWS

ENVIRONMENTAL DATA SERVICE
Asheville, North Carolina, USA 28801

SUBSCRIPTION PRICE: $9.00 a year; $2.50 additional for foreign mailing; single copy price
varies.* Chee! money orders be made payable to the Department of Commerce, NOAA
Remittance and cor ence regarding subscriptions should be sent to the National Climatic
Center, Federal Bu

“PRICE THIS ISSUE .55


1973

September

Boulder HF Doppler Observations

= 90° 80° 0° 90°,

Ss

a

20
oT
1000 = 1200

T T T T T T T T T T T T q T

T
1400 1600 ~—1800 2000 =—2200 «= 2400S 0200 = (0400
Universal Time

No sunlit observations
ssee++ No F-region observations

Figure 7.2 SFD observing time near Boulder, Colorado during
the second manned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

66



Boulder HF Doppler Observations
80° 90°

July

August

5 .
T T T T T T T

f T
1000 1200 1400 1600 =—:1800 = 2000 =. 2200
Universal Time

T T T

T
2400 ©0200»=— 0400

No sunlit observations
++e+++ No F-region observations

Figure 6.2 SFD observing time near Boulder, Colorado during
the first unmanned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

52



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TABLE 9.2

THE IMPULSIVE 10-1030A FLUX ENHANCEMENT DEDUCED FROM SFDs DURING THE THIRD
MANNED MISSION OF ATM SKYLAB

Number of
Channels
. of SFD Data Start Peak
Date Analyzed To Time Time A*(10-1030A)
1973 48 (10-1030A) ur ur
[December 23 2 2332.2 2333.9 aston

* A®(10-1030A) flux units are Watts m7,

10. DISCUSSION

The SFDs and estimates of 10-1030A flux enhancements reported here provide information on the
impulsive EUV flare emissions before and during the ATM-SKYLAB observations. Hopefully these results
will be useful for studying the impulsive flare emissions and the relation of these impulsive
emissions to the slower soft x-ray emissions. These results should also be useful as background
information to scientists studying the ATM observations of the evolution of active regions and the
flare productivity of these regions.

The level of solar activity was relatively low during the ATM-SKYLAB missions. The 10 cm flux
was below 100 most of the time and dipped below 80 to near sunspot minimum values frequently during
the last manned mission. Consequently, the frequency of occurrence of events was lower than during
most of this sunspot cycle. Fortunately, a good solar rotation of flare activity was well observed
with ATM experiments in early September during the second manned mission.

All the EUV bursts observed via SFDs during the ATM observations were more than an order of.
magnitude smaller than the largest events observed from September, 1960 to July, 1970. However,
several nice medium-sized EUV bursts were observed via SFDs. Some of the events had extensive fine
time structure or were quasi-periodic (e.g., 1411 UT June 15, 1973; 2153 UT September 2, 1973; and
1830 UT September 5, 1973). Considering the high spatial resolution and extensive spectral coverage
of the ATM observations, significant advances in our knowledge of solar flares should be obtainable.

Further information on the SFD and 10-1030A results for particular events may be obtained by
writing to Dr. R. F. Donnelly, Space Environment Laboratory, NOAA Environmental Research Laboratories,
Boulder, Colorado, 80302, USA. The absolute accuracy of the 10-1030A flux enhancement varies from
event to event and during events, but is generally about a factor of four. The absolute and relative
timing accuracy also varies from one event to another and from one data set to another. When the
ATM data are analyzed to where the flares observed during the third manned mission are known, it may
be possible to obtain further information on the corresponding SFD observations in England, U.K.,
Alabama and Hawaii, USA.

11. ACKNOWLEDGEMENTS

We gratefully acknowledge financial support as follows: The HF Doppler measurements at Boulder
were made as part of ARPA Order No. 1361. The HF Doppler measurements of the University of Hawaii
Radio Science Laboratory were sponsored by the Atmospheric Sciences Section, National Science Founda-
tion Grant #GA-23964. Analysis of SFDs during the ATM-SKYLAB missions were supported by NASA
Marshall Space Flight Center Order No. H-2532B. We wish to recognize the help of Frank Cowley of the
NOAA Space Environment Laboratory (SEL), who wrote the computer programs used to analyze the SFD and
compute A(10-1030A). We are also thankful for aid in processing SFD and ionogram data to Lois
Wescott of the NOAA Environmental Data Service, Boulder, Colorado; Richard Salaz of the University of
Colorado, and Brian Kutara of the University of Hawaii. John Taylor of the NOAA SEL Instrumentation
Group helped prepare the HF Doppler receiving and recording equipment used at Sacramento Peak
Observatory during the ATM mission. Furthermore, we appreciate the acrobatics of J. Edward Coleman
installing the receiving antennas in the tall pine trees at Sacramento Peak Observatory.

94



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LONGITUDE WEST

Figure 2.5 Locations of transmitters, receivers, and ground paths
for HF Doppler observations in Hawaii.

3. SFD ANALYSIS PROCEDURES

The magnetic tape recordings of frequency deviations in the 0.1 to 100 Hz range are replayed at
speeds from about 25 times up to about 2,000 times the speed at which the data were recorded, where
the lower speeds are used for large SFDs when high time resolution is desired and the higher speeds
are used when searching for the occurrence of events. The speed-up in replaying the data shifts the
frequency range into the audio range. The data are then processed by standard audio spectral
analyzers. Two types of spectra analyzers are usually used. First a Rayspan is employed to make
records of an entire data tape, which usually contains two weeks of data. These records are used in
searching for the occurrence of special events, e.g. SFDs, and to study daily variations. The
latter information is used in the analysis of SFDs by determining the extent of changes in the
ionosphere between the latest available preflare ionogram and the start of the SFD. One can also
tell whether the HF Doppler propagation path is reflected from the bottom of the E-layer or from the
F-layer because the amplitude of the background frequency deviations are much larger in the latter
case than in the former.

Once the times of SFDs are determined, sonagrams like that shown in Figure 3.1 are made for a
small time interval including the SFD for each channel of data. The preflare frequency deviation is
offset from zero by the HF Doppler recording instrumentation so one can distinguish a decrease from
an increase with respect to the average value. Several sonagrams are usually made for each HF
Doppler channel for each SFD for the following reasons. When significant absorption of the HF radio
wave occurs during the solar flare, one playback gain is used to show the preflare and postflare
frequency deviations clearly. A second higher gain is used to show the main part of the SFD, where
now the preflare and postflare period will usually be complicated by minor noise. Higher gains may
then be used for the late portion of the SFD when the soft x-ray and flare-induced absorption are at
a maximum. Slower playback speeds are used to attain higher time resolution, but unfortunately,
while the time scale is increased, the frequency scale is decreased. Nonlinear amplification is
used to generate harmonics of the primary frequency deviation in order to effectively increase the
frequency deviation scale for the harmonics. Some of the SFDs discussed later were scaled from
third or fifth harmonics. The frequency as a function of time f(t) is then digitized for each HF
Doppler channel that observed the SFD clearly, using a Hewlett-Packard scaler and calculator Model
9820A. The frequency deviation Af(t) during an SFD is simply Af(t) = #(t)-f.,where f. is the
preflare value of f(t). ° °

|
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In order to provide worldwide time and frequency standard information, the WWV antennas are
half-wave vertical dipoles that radiate omnidirectionally in the horizontal plane with strong radia-
tion at low elevation angles. The results for the SFD measurements are that radio waves reflected
from the bottom of the E-layer or paths outside the great circle plane of the transmitter and
receiver locations are stronger than ideal. The receiving antennas were half-wave horizontal
dipoles strung about one-quarter wavelength above the ground. The axis of each antenna was oriented
approximately perpendicularly to the great circle plane of the transmitter and receiver locations
which provides a mild directivity in support of great circle propagation paths reflected in the F-
region.

Usually 5 MHz was too low for propagation paths to be reflected from the F-region to Sacramento
Peak, i.e., 5 MHz was normally reflected from the bottom of the E~layer. Usually 15 MHz was too
high a frequency to be reflected in the ionosphere to as short a range as 881 km, i.e., the skip-
distance usually exceeded 881 km. So 10 MHz provided the main measurements of SFDs, but frequently
the only 10 MHz daytime path was reflected from the bottom of the E-layer or sporadic E-layers.

The time and frequency standard station WWVH in Hawaii also transmits at 5, 10 and 15 MHz. The
WWVH antenna patterns are cardioid shaped in a horizontal plane with the minimum radiation in the
easterly direction. Also, the orientation of the receiving antennas at Sacramento Peak Observatory
results in a minimum sensitivity to radio waves from the west. Consequently, reception at Sacramento
Peak Observatory of WWVH was not expected. However, frequently 15 MHz WWVH and occasionally 10 MHz
WWVH were received, as was evident from the voice announcements. The great circle ground range from
WHWVH, Kauai, Hawaii to Sacramento Peak Observatory is about 5,404 km. The WWVH propagation paths
were multiple-hop and may have deviated significantly from the great circle plane. For several SFDs
reported later, 15 MHz WWVH to Sacramento Peak Observatory provided the sole observation of the
event.

No jonograms were available from near the midpoint of the path from WV to Sacramento Peak.
Tonograms were obtained from near the end points of the propagation path, namely Boulder, Colorado,
and from White Sands Missile Range, near White Sands National Monument (see Figure 2.1). For many of
the SFDs observed, preflare ionograms of sufficient quality for computing the ionospheric electron
density as a function of height were not available from White Sands.

The Sacramento Peak HF Doppler observations commenced March 30, 1973 and terminated February 4,
1974, These observations were examined to detect SFDs, first by looking directly at the records and
secondly by checking the data at the times of flares listed in Solar-Geophysical Data. Loss of data
due to equipment malfunction, power failures or the time required to change magnetic tapes totaled
less than 4% of the total observing period, where most of the lost data occurred on November 30,
1973, because of a power failure. Preliminary reports of SFDs observed at Sacramento Peak were
published in Solar-Geophysical Data.

2.2 HF Doppler Observations Near Boulder, Colorado

Figure 2.2 illustrates the geographic layout of an HF Doppler observatory near Boulder, Colorado,
that was operated under ARPA Order No. 1361 to observe moving ionospheric irregularities. Three
paths are used for triangulation of the motions. The observation of SFDs was a fortunate by-product.
The frequencies transmitted from the three stations were offset from each other by about a 1 kHz
interval at 2.4 MHz, 2 kHz at 4.8 MHz and 2.5 kHz at 6 MHz, so the received signals could be recorded
on separate channels, e.g., 4.8 MHz from Fort Collins is recorded on a different magnetic tape than
4.8 MHz from Sunset or 4.8 MHz from Keenesburg. The three transmission frequencies of about 2.4,

4.8 and 6.0 MHz and the three different propagation paths result in nine channels of HF Doppler

data. The main disadvantage for observing SFDs on nearly vertical propagation paths like these is
that time-varying local ionospheric irregularities cause sizeable frequency deviations that constitute
noise relative to the flare-induced frequency deviation. Because the frequency deviations from

local irregularities are not simultaneous while the SFD is simultaneous for the three different
propagation paths, the three sets of data can be used to average out or reduce the noise from local
irregularities.

Usually during the daytime, 2.4 MHz was reflected from the bottom of the E-layer and was
therefore insensitive to the 10-1030A flare radiation. During June (first ATM manned mission), 6
MHz was usually too high a frequency for reflection from the ionosphere for such short path lengths.
For many of the SFDs, 4.8 MHz was reflected only as an extraordinary wave because the ionosphere
peak electron density was too low for reflection of the ordinary wave. The nine channels of Boulder
HF Doppler data for the period April 1, 1973 through February 3, 1974, were searched for SFDs. Iono-
grams recorded at Boulder were used to determine the preflare electron density as a function of

eight.

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92


7. OBSERVATIONS DURING THE SECOND MANNED MISSION OF ATM-SKYLAB

The second manned ATM observing period (August 7 to September 21, 1973) was the richest in
number of solar flares, although the number of flares was much lower than in the two month period
before the ATM mission discussed in Section 4. The level of solar activity rose from low levels,
comparable to those of sunspot minimum years, in mid-August, to moderate levels in the first week in
September. The Ottawa 10 cm flux reached a daily average of 136.5 on September 3. The observed
SFDs are listed in Table 7.1 and the computed flux enhancements are in Table 7.2. All the 10-1030A
bursts were small in intensity (A9(10-1030A) < 5x10-4 Watts m7“), except for the medium sized burst
of 0945 UT September 4, 1973. Several events show complex fine structure or are quasi-periodic
(September 4 and 5). The periods of SFD observations at Sacramento Peak Observatory and near Boulder
are indicated in Figures 7.1 and 7.2 respectively. The daily SFD observing period shortens from
summer to fall, but the periods of reduced sensitivity due to the propagation path being reflected
from the bottom of the E-layer or from sporadic E are also shorter and less frequent.

Some of the SFDs used to compute A(10-1030A) were noisy or of poor quality, but they were
nevertheless analyzed in detail if they were also observed by the ATM experiments. Similar events
in Section 4 were not used to compute A6(10-1030A). To help clarify what portions of the results
may be noise from what must be a real flare enhancement, results from several different channels of
SFD data are shown. The results in Table 7.2 are an average over all channels processed, including
some not shown in the Figures. The best events from the viewpoint of having interesting impulsive
fine structure observed by good SFD data are those on September 4 and 5.

The long lasting 2B flare of 1140 UT September 7, 1973, was probably the largest event of the
second manned mission. Figures 7.1 and 7.2 show that this flare occurred too early for SFD observa-
tions at Sacramento Peak Observatory or near Boulder. The SFD was observed in England to be a long
lasting sequence of small impulsive peaks (see Table 7.1) superposed on a long lasting gradual en-
hancement. The associated microwave bursts exhibited a large impulsive rise at 1156 UT, with impul-
sive fine structure peaks lasting until 1207 UT. Any corresponding EUV bursts were not observed in
the SFD data because the large soft x-ray enhancement associated with this flare had enhanced the
ionospheric absorption (SWF) of the HF Doppler radio waves so much that the data in England were lost
just before 1155 UT, at which time the data did not yet indicate the occurrence of any increase.

60



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47


6. OBSERVATIONS DURING THE FIRST UNMANNED MISSION OF ATM-SKYLAB

The last ATM film observations of the first manned mission (SKYLAB II) were taken on June 18, 1973,
and the first film observations of the second manned mission (SKYLAB III) were taken on August 7, 1973.
The interim period, June 19 through August 6, will be discussed here. The Harvard ATM experiment made
observations via telemetry during this unmanned period.

The SFD observing times are shown in Figures 6.1 and 6.2. The Sacramento Peak observations were
reduced in sensitivity most of the time by the dominance of HF Doppler propagation paths reflected
from the bottom of the E-layer of the ionosphere. The level of solar activity was generally low during
this period. Although the daily average Ottawa 10 cm flux did rise above 100 from June 20 through 26,
it dipped below 80 to nearly sunspot minimum values in mid-July and early August. The observed SFDs
are listed in Table 6.1 and the peak 10-1030A flux values for some of the larger SFOs are,listed iny

Table 6.2. All of these EUV bursts are of small intensity, i.e., AG nay (10-1030) < 5x10°" Watts m%.

WWV Sacramento Peak Observatory
HF Doppler Observations

80°90°
jo

August

T t
1000 = 1200-=— 400

t t t t T
1800 2000» 2200» 2400» 02000400

Universal Time

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1600

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tttt++No F-region observations

Figure 6.1 SFD observing time at Sacramento Peak Observatory
during the first unmanned observations with ATM.

Clear areas indicate good observations, dotted indicate re~
duced sensitivity, solid line indicates no observations.

51

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13

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ATM ATM ATM
Manned Manned Manned
Observations Observations Observations

1 29 18 7 2i 26 3
April May June August September November February
1973 1973 1973 1973 1973 1973 1974

| i | 4 1 {

r T T T T t
Atlas a

Section: 4 5 6 7 8 9

Figure 1.1 Observation periods.

2. HF DOPPLER OBSERVATIONS

Measurements of frequency deviations on HF radio waves reflected from the jonosphere are
called HF Doppler measurements. The 0.1 to 100 Hz range of frequency deviations are recorded on
magnetic tape along with time codes. The instrumentation used is like that described by Baker
et al. [1968]. A variety of events other than SFDs are observed in HF Doppler measurements. Some-
what different HF Doppler experiments are conducted according to the type of event to be studied.
The ideal experiment for observing SFDs consists of a ground-range separation between transmitter
and receiver of about 600 to 1200 km so that the horizontal length of the radio wave propagation
path is long enough relative to local time-varying ionospheric irregularities to average out their
contribution to the observed frequency deviation. Longer paths are undesirable because multiple-
hop paths occur and it is difficult to accurately determine their ray paths. Transmitter and
receiver antennas should be quite directional along the great circle path between the transmitter
and receiver stations to suppress propagation paths that deviate significantly from the great circle
plane of the transmitter and receiver stations. The receiver and transmitter antennas. shoulg also
be directional in the vertical plane with the main beam at elevation angles in the 15° to 27° range
in order to enhance one-hop propagation paths reflected in the F-region of the ionosphere because
such paths are sensitive to the ionospheric effects of flare radiation in the full 1-1030A wave-
length range. Both antennas should have low gain at elevation angles below 15° in order to suppress
one-hop paths reflected from the bottom of the E-layer, or from sporadic E-layers. Such paths are
sensitive mainly to the ionospheric effects of 1-10A soft x-rays that are routinely well observed by
satellites. Similarly, the antennas should have low gain at elevation angles above about 30°in
order to suppress multiple-hop paths because it is more difficult to determine accurately their ray
paths. Ideally, an ionosonde station should be located at the midpoint of the path in order to
provide measurements of the electron density as a function of height just before flares. The
stations should be at equatorial or low midlatitudes since the magnitude of SFDs decreases with
increasing solar zenith angle. About five different transmission frequencies, e.g., 8, 9, 10, 11
and 12 MHz, should be used to insure that, at any particular time, at least one of the propagation
paths is one-hop with a true reflection height near 200 km.

An oblique-path experiment has several advantages relative to near-vertical path experiments.
First, the effects of time-varying local ionospheric irregularities, which are unrelated to the
flare effects and which may produce frequency deviations as large in magnitude as small SFDs, are
smoothed out in oblique-path observations of frequency deviations. Secondly, higher frequencies are
used on oblique paths which suffer less absorption in the ionosphere. Thirdly, the ground wave is
not received on long paths while on short paths it must be nulled out as much as possible by the
antenna patterns. The flare-induced ionospheric absorption of radio waves is less of a problem for
the oblique path than for a vertical path. For an SFD accompanied by a large SWF (short wave fade-
out, or flare-induced enhancement of D-region absorption of HF radio waves), the vertical-path
observations show the SFD until the strength of the ionosphere-reflected radio wave is so weak
relative to the residual signal from the ground wave that the latter dominates and consequently the
receivers stop automatically increasing their gain to track the SFD signal. A fourth advantage is
that the propagation paths are less influenced by the earth's magnetic field because of the higher
frequencies.

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Table 4.2 lists the times and flux values of up to three peaks in A¢(10-1030A, t). When more
than one channel of data were used to compute A6(10-1030A, t) (see column 2 in the table), the times
and flux values were averaged to obtain the results in Table 4.2. The peak flux values and peak times
from different channels agreed quite well, usually to within 10% of the average value or to within
two seconds respectively, although the flux results for the May 5 event range 70% from the average
value. For each event in Table 4.2, all available SFD observations were compared to help determine
noise and non-flare variations in Af(t), even for the cases where only one channel was carried through
to computing A®(10-1030A, t). The underlined flux value is the maximum value for that flare event.
Some flares had slow peaks, which were larger and later than the impulsive values given in Table 4.2,
‘that are not listed in Table 4.2 because SFDs do not provide accurate estimates for such slow
emissions. Two of the events listed in Table 4.2 vary slowly near their maxima and therefore their
peak time is less accurately known. Many of the events in Table 4.1 do not appear in Table 4.2 and
were not analyzed to compute Ao(10-1030A) because the SFD was either not large enough, not of suffi-
cient quality, not from an F-region path, the solar zenith angle was too large, or a large SWF caused
the SED data tobe lost. None of the events is a large EUV enhancement, i.e., (A®, a (10-1030A) =
2x10” Watts m“) [Donnelly, 1970]. The largest (1716 UT May 5, 1973) is more than order of
magnitude smaller than the largest events observed from 1960 to 1970, e.g., 1328 UT November 12, 1960;
1527 UT August 28, 1966; and 1841 UT May 23, 1967 [Dgnnel ly, 1970]. Five of the EUV bursts are in
the medium class (5x 10-4 < A®,,.(10-1030A) < 2x10°~ Watts m72),

Figure 4.3 shows the SFD of 1535 UT April 1, 1973; and Figure 4.4 shows the Ao(10-1030A, t)
estimate that was computed from the SFD using a model for a f. (h) used previously in analyzing SFD data
(Donnelly, 1968], herein called Model 3. These A0(10-1030A9 fesults are our best estimate relative
to results based on Models 4-7. Models 4, 5, 6 and 7 refer to models of Gope that are equal to

1
's iP , ¥2, and 2 times the Gere of Model 3 respectively. Models 4-7 are intended only to demonstrate

the sensitivity. of A6(10-1030A, t) to the assumed ionospheric electron joss rates. Results using
Model 2 based on a pelh) and B.e¢(h) models of Mitra and Banerjee [1971] are shown for several events
Tater in the atlas®’*the value®SF t.¢¢ in Figure 4.4 is unusually high and results from the height
of reflection being very high. e

The remainder of the chapter presents figures of the SFD observations and derived Ao(10-1030A, t)
estimates. Information on the associated Ha flares and microwave bursts are presented below the
figure of the SFD, along with comments on any complications involved in the calculation of A6(10-1030A,t).
When no comments to the contrary are made, the radio wave was an ordinary wave, the HF Doppler propa-
gation path was adequately determined, and t(h) was approximately constant over the range from ho to
hp. The 46(10-1030A, t)/Ao curves are dotted below 0.05 to signify less accuracy for such small
values. These curves are sofiétimes also dashed late in the flare to signify lower accuracy of the
flux estimate than for the solid line. Calculations were made using Models 2-7 but best-estimate
AG(10-1030A, t) results based on Model 3 are the only ones presented here, in order to conserve space.
Similarly, results for only one channel of SFD are presented. More extensive results are given later
for flares during the ATM observing periods. The exception to these two limitations are the results
for the flare of May 18, 1973, shown in Figures 4.27 - 4.38, That SFD was selected for detailed
illustration because it includes a long duration slow component which is small in Af(t) yet large in
40(10-1030A, t). It is therefore an excellent event for demonstrating how well SFDs determine the
impulsive EUV emission and how poorly the slow 10-1030A enhancement, as a function of transmission
frequency, path length of the HF Doppler radio wave, and the assumed ionospheric electron loss rates.
Discussion of these features is included below the captions of Figures 4.27, 4.29, 4.31, and 4.33.

No estimates of A® (10-1030A) were made for the 2B flare of 2100 UT April 29, 1973, because
all the available HF DofBter data were lost due to the large SWF from the soft x-ray enhancement.
The HF Doppler traces were lost before any impulsive SFD structure was detected. The 2-35 GHz micro-
wave burst was the largest observed during the periods covered in this atlas. Another type of iono-
spheric observation that is sensitive to the 1-1030A flare radiation is the measurement of total
columnar ionospheric electron content using geostationary radio beacons, where the observed flare
effect is called a SITEC. The observed SITEC for this flare was quite large. The time rate of
change of the total columnar ionospheric electron density was comparable to that for the flares of
ton) April 11, 1973 and 1716 UT, May 5, 1973 (R. Fritz, NOAA, Boulder, Colorado, private communica-
tion).

20



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23


1973

1974

Boulder HF Doppler Observations

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peveee No F-region observations

Figure 9.2 SFD observing time near Boulder, Colorado during
the third manned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

90

|
|



Table 5.2 The Impulsive 10-1030A Flux Enhancements Deduced From
SFDs During the First Manned Mission of ATM-SKYLAB
May 29 - June 18, 1973

Number of
Channels of
SFD Data Start Peak Peak
‘ Date Analyzed to Time Time g(10-1030A)* Time  4$(10-1030a) *
1973 48 (10-1030A Ur Ur Peak ur Peak
ol,
June 15 4 1407 1410.9 7.1x10
- 4
June 16 1 qhal.4 1423.2 2.0x107" 1hek.5 — 3.1x10 * .

Underlined peak flux values are the maximum values for the event.

*)8(10-1030A) flux units are Watts mTM°.

The quality of the SFD data for the SFDs illustrated in Figures 5.3, 5.10 and 5.12 is generally
lower than for the events selected for illustration in Section 4. The June 15th event was quasi-
periodic (10.4 sec) and had the largest peak 10-1030A flux enhancement of all the SFDs observed during
the ATM missions. It was a medium sized 10-1030A burst, comparable to the larger events in Table 4.2,
but more than an order of magnitude smaller than the largest events observed during 1960 to 1970. The
ATM observations of this flare commenced their flare mode just after 1411 UT, so the impulsive phase
of the flare was missed but the rising slow component was well observed.

44



8. OBSERVATIONS DURING THE SECOND UNMANNED MISSION OF AT ATM-SKYLAB

The last ATM film observations of the second manned mission (SKYLAB III) were taken on
September 21, 1973, and the first film observations of the third manned mission were taken after 1900
UT on November 26, 1973. Because the SFDs observed in Boulder on November 26 occurred before 1900 UT,
we have designated September 22 through November 26 as the second unmanned period of ATM observations.
Some ATM observations were made during this period, e.g., by Harvard's experiment; however, it is very
unlikely that ATM observations were made during the impulsive phase of solar flares.

The SFD observing times at Sacramento Peak Observatory and at Boulder are shown in Figures 8.1
and 8.2, respectively. The Boulder data were lost on October 8. The level of solar activity was quite
low. The daily average 10 cm flux dipped below 80 to nearly sunspot minimum values from October 9
through 20, and from November 4 through 20. Relatively few solar flares occurred during the second
unmanned mission. The few SFDs observed are listed in Table 8.1. All of these SFDs were small or of
poor quality; therefore Ad(10-1030A, t) was not computed for any of the events. In general the SFD
observations in Hawaii were better than at Sacramento Peak and Boulder for this period. It is very
fortunate indeed that no manned ATM mission occurred during this period so barren of solar activity
of terrestrial significance.

WWV Sacramento Peck Observatory
HF Doppler Observations

“X= 90°80°
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September

October

1973

November

T T T T T1111 T
1000 1200 1400 16001800 2000 ©2200» 2400» 0200» (0400

Universal Time

‘No sunlit observations
+ No F-region observations

Figure 8.1 SFD observing time at Sacramento Peak Observatory
during the second unmanned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

85



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Figure 8.2 SFD observing time at Boulder, Colorado during
the second unmanned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

86



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Pigure 2.3 Locations of transmitters, receivers and ground paths
for HF Doppler observations at Leicester, Mngland.

2.3 HF Doppler Observations in England

HF Doppler observations are made at the University of Leicester in England in order to study
traveling ionospheric disturbances that are excited in the auroral region and travel toward the
southeast over England. Four nearly vertical propagation paths are used. The ground paths are
shown in Figure 2.3. The four transmissions are separated by 3 Hz intervals and are therefore
observed by one receiver. The individual frequency deviations are separated through frequency
spectral analysis. These observations were studied for several of the solar flares observed by ATM-
SKYLAB at times too early for SFD observations in Boulder or Sacramento Peak Observatory. Ionograms
from Slough, just west of London, were used to estimate the preflare ionosphere over Leicester.

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Most of the HF Doppler observations discussed below were intended to observe frequency-deviation
events other than SFDs, e.g., traveling ionospheric disturbances (TIDs) due to aurora sources,
severe storms, or static rocket test firings, etc. Consequently, most of the observations were made
with nearly vertical paths and the SFD observations were a fortunate by-product. Table 2.1 quanti-
tatively presents the geographic locations, path lengths and frequencies of the HF Doppler observa-
tions studied. All of the observations were processed by sub-audio frequency spectral analysis,
which permits detection of SFDs as small as 0.1 Hz peak frequency deviation and separation of two:
different signals with frequency deviations that differ by more than about 0.1 Hz when processed
with time resolution of several seconds.

TABLE 2.1
SFD Observatories
Receiving Station Transmitter Station Received Great-Circle
Name and Frequencies Ground Range
Geographic Coordinates Name Geographic Coordinates MHz km Comments
Sacramento Peak Observatory WV 40°40'49,0"N 105°02'27. 5, 10, 15 881 Operated to observe SFDs
32°47'12"N 105°49'12"W during ATM-SKYLAB.
WIVH 21°59'26.0"N 169°46'00.0"N 10, 18 5,404 Observations from April 1,

1973 to February 4, 1974
were thoroughiy searched for
SFOs. Preliminary reports
or observed SFOs were pub-
lished in Solar-Geophysical

Data.
Table Mountain, Sunset  40°2'25"N 105°27'5"N 2.4, 4.8, 6.0 20.5 Observations from April 1,
Boulder, Colorado 1973 to February 4, 1974
40°7'42"N 105°14'18"W Keenesburg 40°4'30"N 104°30'30"W were thoroughly searched for
62.7 SFDs.
Fort
Collins — 40°35'0"N 105°9'30"W $1.1
Leicester, England Four 4.793 66 to 90 SFOs for certain flares
52°23'N 1°3'W Stations observed by ATM-SKYLAB
Near 52.4°N 1°W were studied in detail.
Gainsborough, Upwood, Bicester
and Stafford, England
Marshall Space Flight Nicka- 35°1'N 85°37'W 4.0125 94 SF0s for certain flares
Center jack observed by ATM-SKYLAB
Huntsville, Alabama Dam were studied.
34°43'N 86°35'W
Muscle 34°47'N 87°37'W 4.759 95
Shoals,
Alabama
Fort Me-33°44'N 85°44'W 5.374 134
Clellan,
Alabama
Honolulu, Oahu, Hawaii WHVH — 21°59'26.0"N 159°46'00.0"N, 5, 10 216 SFDs are routinely scaled
21.3°N 157.5°0 and reported in Sotar~
Geophysical Data.
Hana, Maui, Hawaii WWVH — 21°59'26.0"N 159°46"00.0"" 5, 10 410 SFDs for certain flares
20.8°N 156.0°H observed by ATM-SKYLAB
were studied in detail.
Kona, Hawaii, Hawaii WIV 21°59'26.0"N 159°46'00.0"W 5, 10 470

19.6°N 156.0°H

2.1 HF Doppler Observations at Sacramento Peak Observatory

HF Doppler receivers were installed at Sacramento Peak Observatory to receive the frequency
standard transmissions of station WWV at 5, 10, and 15 MHz in order to measure SFDs during the ATM-
SKYLAB missions. Figure 2.1 shows the locations of the transmitters and receivers. The ground
range of 881 km is ideal. The WHY transmissions were used because funds were not available to
operate separate transmitters. WHV transmits 10 kW of power at each of the three frequencies
received at Sacramento Peak Observatory.



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Figure 3.1 The sonagraph record of the SFD of 1843UT April 11, 1973.

The procedure used to calculate the 10-1030A flux enhancement (A%) for all the results in this
atlas was method 3 of Donnelly [1970, p,75]. It is the most suitable method for application to a
large number of events. This method involves two main related simplifying assumptions, namely (1)
that the time rate of change of electron density (dN./dt) in the ionosphere during the solar flare
is approximately constant with height from just abové the bottom of the E-layer (h,) to the height
of reflection (h,,) and (2) the electron loss time constant t(h) is approximately constant with
height over the range from hy to h.. The first assumption is approximately satisfied at heights
below about 200 km if the second assumption is true and because the EUV flare spectrum is spread
over the 10-1030A range in continuum emission and in a large number of emission lines. This spread
spectrum leads to the rate of production of ionization being roughly constant in the 110 to 200 km
altitude range. The second assumption is not strictly valid for some of the events, so those
cases are identified later in the atlas. For those events of particular relevance to the ATM-SKYLAB

observations, the sensitivity of the results to the assumed effective electron-loss time constant is
illustrated.

The first assumption simplifies the relation between Af and AN, /dt [Agy et at., 1965], namely

dt

(1)

in the altitude range from hy to hy, where k = 80.6 Hz?m?, fy is the equivalent vertical incidence
frequency, c_ is the speed of light and h*), is the virtual height of reflection. Transmission curves
[Smith, 1939] and ionograms taken just before the flare at a location near the HF Doppler propaga-
tion path were used to determine hp, hg and fy for each event and channel analyzed.

Equation (1) was evaluated numerically and also integrated from the start of the event to time
t to determine ANg(t) in the upper E- and Fl-region of the ionosphere. The rate of flare-enchanced
production of iontzation Aq(t) was then computed for an effective electron loss time constant t fF
from the electron continuity equation, e

dN AN
2
Aq(t) = ae + f+ Boece (AN) (2)
cia Tort ef fNe
AN

The nonlinear term in (2) was small relative to the = term for all the flares discussed in this
atlas.

The energy flux enhancement was then computed from

A0(10-1030A,t) = a sec (x) Aq(t) (3)



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UAG-33

UAG-34

UAG-35
4

"Auroral Electrojet Magnetic Activity Indices AE(10) for 1967", by Joe Haskell Allen, Car
C. Abston and Leslie D. Morris, National Geophysical and Solar-Terrestrial Data Center,
Environmental Data Service, May 1974, 142 pages, price 75 cents.

"Absorption Data for the IGY/IGC and IQSY", compiled and edited by A. H. Shapley, Nationa
Geophysical and Solar-Terrestrial Data Center, NOAA, Boulder, Colorado, U.S.A., W. R.

Piggott, Science Research Council, Slough, U.K., and K. Rawer, Arbeitsgruppe fiir Physikalische
Weltraumforschung, Freiburg, G.F.R., dune 1974, 381 pages, price $2.00.

"Catalogue of Digital Geomagnetic Variation Data at World Data Center A for Solar-Terrestrial

Physics", prepared by Environmental Data Service, NOAA, Boulder, Colorado, July 1974, 20 pages,
price 20 cents.

USCOM-NOAA~ASHEVILLE=10-30-74=650



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where x is the solar zenith angle at the midpoint of the propagation path at the time of the peak of
the event and a = 6.56x107** Watt-m-sec. [Donnelly, 1970].

The values of tere and Begg were determined from models of a, pel) Berf(h). The electron density
as a function of height was coiéutated for each flare and HF Doppler observatory using the correspond-
ing preflare ionograms and the methods of Wright [1967]. The true height of reflection hy was then
determined from Ne(h), where Ne(hr) = f§/k. Using several models of og¢¢(h) and Bege(h), including
those of Mitra_and Banerjee [1971], t and B were computed as a function of altitude from z(h) =
[2de¢¢(h)Ne(h)]~?, or c(h) = Bu! at the higher altitudes, and B(h) = ag¢¢(h), or B (h) = 0 at
altitudes where 8 applies. Averages of t(h) and B(h) were computed over the height range from hg to
hp to determine tere and Borf.

The Agnax(10-1030A) values computed using method 3 are estimated to be accurate to within a
factor of four [Donnelly, 1970]. The impulsive structure in A&(10-1030A, t) with time constants less
than tef¢ (see (2)) are insensitive to the height variations of t or to the a(h) and g(h) models,
while the flux variations with time variations larger than Teff are quite sensitive. lIonospheric
variations unrelated to the solar flare effects produce noise in the SFD observations that mainly
affect the A®(10-1030A) estimates during the slow flare emissions. SFD data provide good informa-
tion on the impulsive emissions of flares, poor information on the slow flare emission, and no in-
formation on the nonflare solar radiation.

4. OBSERVATIONS DURING TWO SOLAR ROTATIONS BEFORE THE ATM-SKYLAB

In order to provide background information on the EUV flaring of the active regions whose rem-
nants were observed during the first manned mission of ATM, and to place the EUV bursts during the
ATM observations in perspective, the SFD observations from April 1 to May 28, 1973 will be discussed.
The Zurich relative sunspot numbers in April and May were lower on the average than in 1967 through
1972, but were generally higher than during the first and third manned ATM observations. The sunspot
numbers during the first week in September during the second period of manned ATM observations
exceeded the sunspot numbers in April and May; however, this pre-ATM period was richer in large EUV
bursts, at least during the daylight observing period of the SFD observations studied.

Figures 4.1 and 4.2 demarcate the periods when SFDs (Af__>0.2Hz) could have been observed on
at least one of the HF Doppler data channels at Sacramento paar Observatory and near Boulder,
respectively. Sunrise in the ionosphere preceeds sunrise at the ground. The dotted lines indicate
the times when all the channels of received transmissions were dominated by paths reflected off the
bottom of the E-layer or sporadic E-layers. Such propagation paths are much less sensitive to EUV
bursts than propagation paths reflected in the F-region because they involve only the ionospheric
effects at heights below about 110 km produced mainly by the 1-10A flare radiation. Hence, the
dotted lines mark periods of low sensitivity for detecting SFDs. Once an SFD is detected, further
spectral analysis of oblique path data with high gain may bring out a larger SFD on a weaker F-region
path in spite of the strong E-region path. In Figure 3.1, the E-region path is weaker than the F-
region path and is lost due to the large flare-induced absorption enhancement (SWF).

The frequency deviations caused by the rising sun and the transient build-up of the ionosphere
are of the order of 1 Hz and complicate the detection of SFDs. Large solar zenith angles (x) reduce
the magnitude of the SFD for a given strength of EUV burst. For x < 85°, Af = cos y. Usually,
SFDs are not analyzed for y = 80° because the frequency deviations are small, because the ionosphere
cannot be adequately approximated as a horizontally or spherically stratified medium, and because x
and the background frequency deviaitons and nonflare ionization are time varying. Sunset at the
ionospheric heights of the HF Doppler paths does not produce a distinct signature in the frequency
deviations, so x = 90° was used as a practical end to SFD observations.

Table 4.1 lists the main features of SFDs observed. Note that some events have results listed
for more than one transmission frequency or receiving station. These were cases that were analyzed
in detail. Secondary peaks are listed when their peak frequency deviation was greater than one-third
the maximum value and the adjacent valleys were less than two-thirds that particular peak. The time
of a peak in the frequency deviation marks the time of impulsive structure in the 10-1030A radiation,
j.e., either a peak-in the radiation or the end of rapid rise, which may then be followed by a slow
rise in the radiation and a slow decrease in the frequency deviation. The time of the main zero
crossing is important in that A®__ (10-1030A) will occur at or before the main zero crossing and at
or later than the maximum frequency deviation. The start time in the case of initial gradual rises
may vary from one SFD channel to another by about one minute, depending on the background of frequency
deviations unrelated to flares. The end time of an SFD is usually very uncertain, since the SFD
frequency deviation approaches asymptotically the background non-flare variations. The SFD end time
probably preceeds the end of the 10-1030A flare radiation. Although the magnitude of Ad (10-1030A)
is usually proportional to Af_., their relation also depends on the solar zenith angle, PRSnsmission
frequency, and the path of the°AF Doppler radio wave in the ionosphere. SFDs observed on paths
reflected from the bottom of the E-layer (see comment 15 in Table 4.1) have small Afingx Values

relative to A® x(10-1030A) . Note that several of the SFDs are classified as large (OFnax 24.5 Hz).
None of the SF ‘during ATM-SKYLAB was that large.

an



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

UAG-32

"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-Terrestria
Physics, November 1972, 128 pages, price 70 cents.

“Auroral Electrojet Magnetic Activity indices (AE) for 1970", by Joe Haskell Allen, Nationa
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,

probed 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, Car
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, price 75 cents.

"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, E1 Segundo,
California, 90245, April 1974, 26 pages, price 35 cents.

|
c



1973

August

September

WWYV Sacramento Peak Observatory
HF Doppler Observations

5 90"80",

50°90"

2 FF.

T i i

1000 1200 = 1400

1600 1800

Universal

No sunlit observations
sse+** No F-region observations

a
2000 ©2200 =. 2400 = 0200
Time

0400

Figure 7.1 SFD observing time at Sacramento Peak Observatory
during the second manned observations with ATM.

Clear areas indicate good observations, dotted indicate re-
duced sensitivity, solid line indicates no observations.

65


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50


AGY, V., D. M. BAKER,
and R. M. JONES

BAKER, D. M,

N. CHANG, K. DAVIES,
R. F. DONNELLY and
J. E. JONES

DONNELLY, R. F.

MITRA, A. P., and
P. BANERJEE

REEVES, E. M.,
R. W. NOYES and
G. L. WITHBROE

SMITH, N.

WRIGHT, J. W.

1965

1968

1970

1971

1972

1939

1967

REFERENCES

Studies of solar flare effects and other ionospheric
disturbances with a high frequency Doppler technique, NBS
Tech. Note No. 306 (U. S. Government Printing Office,
Washington, D. C.).

A review of some ionospheric studies based on a high-frequency
Doppler technique, ESSA Tech. Rept. ERL 78-SDL 1 (U. S.
Government Printing Office, Washington, D. C.),

Extreme ultraviolet flashes of solar flares observed via
sudden frequency deviations, ESSA Tech. Rept. ERL 169-SDL 14,
(U. S. Government Printing Office, Washington, D. C.).

Models for the effective recombination coefficients in the
ionosphere, Space Res. XI, ed. K. Ya. Kondratyev, M. J.
Rycroft and C. Sagan (Akademie-Verlag, Berlin), 1019-1025.

Observing programs in solar physics during the 1973 ATM SKYLAB
Program, Solar Phys., 27, 251-270.

The relation of radio sky wave transmission to ionosphere
measurements, Proc. IRE, 27, 322.

Tonospheric electron-density profiles with continuous
gradients and underlying ionization corrections. III Practi-
cal procedures and some instructive examples, Radéo Set., 2
(New Series), 1159-1168.

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