The data reduction procedures and programs for analysis of the IMP F and G energetic particle flux experiments are summarized. The IMP-F experiment contained two thin-window Geiger-Mueller detectors and an ionization chamber. There were two IMP-G experiments: one with six Geiger-Mueller detectors and an ionization chamber, and the other with two funnel mouthed channeltrons in a parallel plate electrostatic analyzer. These experiments measured particles in the energy range above 20 keV (IMP-F) and above approximately 5 keV (IMP-G). A bibliography is presented of papers containing the scientific results. These data were predominantly used for the study of low energy solar particles from flares

Anderson, K. A.

English

NASA Technical Reports Server

n t- / Energetic Particle Flux Experiment
H CO
0 January 28, 1965- June 30, 1971
o
to FINAL REPORT
a Addendumto Final Technical Report
. NAS,5-9091
Principal Investigator: K. A. Anderson
In -
'April, 1973
O. - Series 14 Issue 19
0UNIVERSITY OF CALIFORNIA, BERKELEY
https://ntrs.nasa.gov/search.jsp?R=19740010223 2020-03-23T10:47:23+00:00Z
Energetic Particle Flux Experiment
(IMP F & G)
January 28, 1965 - June 30, 1971
Final Report
Principal Investigator
Kinsey A. Anderson
April, 1973
Space Sciences Laboratory Series 14 Issue 19
7
TABLE OF CONTENTS
Abstract ii
I. Description of the Data Supplied to the National
Space Science Data Center 1
II. IMP 4, 5 Major Computer Processing Programs 5
III. List of Publications Reporting Results From
IMP-4 and 5 Satellites 7
IV. Papers Presented at Scientific Meetings Reporting
Results From the IMP-4 and 5 Satellites 9
Table 1 2
Table 2 4
Abstract
This report summarizes the data reduction procedures and
programs for analysis of the IMP F and G Energetic Particle Flux
Experiments of the University of California. The IMP-F experiment
contained two thin-window Geiger-MUeller detectors and an ionization
chamber while there were two IMP-G experiments, one with six Geiger-
Mileller detectors and an ionization chamber, and the other with two
funnel mouthed channeltrons in a parallel plate electrostatic analyzer.
These experiments measured particles in the energy range above 20
keV (IMP-F) and above -'5 keV (IMP-G).
The scientific results are summarized in the attached biblio-
graphy of publications. The data from these experiments were predomi-
nantly used for the study of low energy solar particles from flares.
Dr. R.P. Lin and Mr. R.E. McGuire participated in many of
the IMP F & G studies while students in the Ph. D. program.
1.
I. Description of the Data Supplied to the National Space Science
Data Center
The IMP-4 data was supplied to the National Space Science Data
Center in the form of 24 hour plots (1 inch/hour) of the counting rate of
the three detector channels. These plots were generated by FPLT24
(described in section II).
The IMP-5 data was supplied in the form of magnetic tapes. These
were produced by the CDC 6600 program Sl EDIT written by G. Pitt and
G. Sessler. The program in part checked the timing information for
consistency, removed redundant data due to receiving station overlaps and
calculated corrected counting rates for the GM detectors and counting rate
for the Ion Chamber. An output tape containing the rates and refined tra-
jectory data was produced for each orbit. These tapes were then merged
so that five orbits were contained on one reel. The tapes were recorded
at 800 bpi, in odd parity (binary), multifile with two file marks to indicate
the end of information. Each file contains the data from one 24 hour period.
Table 1 describes the format in detail. Table 2 gives the dead time factors
used in calculating the GM corrected counting rates.
2.
Table 1
IMP-5 Edited Tape Format
Word Format
1 Day Integer
2 Time in Ms I
3 Psuedo sequence count I
4 ID or E 2 counting rate in CTS/sec Floating point
5 ID or P2 counting rate in CTS/sec F
6 IC counting rate in CTS/sec F
7 E 1 or E 3 counting rate inCTS/sec F
8 Pl or P 3 counting rate in CTS/sec F
9 IC counting rate in CTS/sec F
Words 10-108 repeat words 1-9 for a total of 12 sequences
109 Orbit day I
110 Ms of day I
111 Geomagnetic latitude (MLAT) F
112 Satellite distance in Km ., F
113 XSE F
position of satellite
114 Y in solar ecliptic F
SE coordinates
115 ZSE F
116 XSM Fposition of satellite
117 YSM in solar magnetospheric F
coordinates
118 ZSM F
119 McIlwain L parameter F
120 Ecliptic Longitude (ELONG) in degrees F
121 Solar Magentospheric Latitude F
(SMLAT) in degrees
3.
Notes
1. ELONG = tan-1 YSE
XSE
SM
-12. SMLAT = tan-I
XSM + SM
3. ID is indicated by a word equal to -1.(floating point).
4. Missing data is indicated by a word of all bits on.
5. All words are in CDC 6000 series standard 60 bit integer or
floating point format.
4.
Table 2
Counter Dead Time Factor (Is)
El 75
E2 100
E3 110
P1 40
P2 95
P3 107
The formula for calculating the corrected counting rate is as follows:
RoR = -TR
where
R = corrected rate
R = uncorrected (raw) counting rate
T = dead time factor for the counter in seconds
5.
II. IMP 4, 5 Major Computer Processing Programs
The following is a description of the major computer programs
written to process the IMP-4 and IMP-5 UCAL experimental data. Al-
though slight variations may exist between the version for the different
experiments they are similar enough to describe as a whole.
1. RATE Program
The RATE programs served as the initial processing step on the
GSFC supplied experimental data tapes. They produced printout (and later
microfilm) containing raw counts and counting rates as seen by the exper-
imental detectors. They also produced cards describing the quantity and
in some sense the quality of the data covered. The programs were written
by Barbara Watson for CDC 6000 System.
2. DATACO F and G
The DATACO programs produced Cal-Comp plots showing the
amount of time covered by each file on the GSFC supplied tapes. Input
is from cards produced by the corresponding RATE program. The following
descriptions apply to IMP-4 programs only.
3. FPLT24 and FPLT6
These programs produce 1 inch/hour and 4 inch/hour by 5 cycle
semi log plots of the GM and ion chamber outputs. The 24 hour plot
serves as the primary display of the IMP-4 experimental data. The
programs were written for CDC 6000 series systems by Maria Roberts
in June, 1967.
6.
4. FV RATE
This program calculates corrected rates and a simple running
average of the corrected rates for the IMP-4 GM counter. It additionally
calculates the ion chamber rate and various spectrum parameters. The
program was written by George Pitt in July, 1967.
The following descriptions apply to IMP-5 programs only.
5. SlEDIT
The Sl EDIT program served as a basic display of the IMP-5 GM
and ion chamber data. It produced two 24 inch by 5 cycle semi log Cal-
Comp plots for each 24 hours of data. In addition it produced an edited
tape containing continuous, non-redundant, time corrected experimental
outputs. These tapes were used as input to further analysis programs and
later supplied to the National Space Science Data Center. S1 EDIT was
written by Gladys Sessler and George Pitt in June, 1969.
6. IMP-5 plotting/averaging system
The system consisted of a collection of programs written by Carl
Wittnebert in February, 1970. It produced Cal Comp plots of averaged
data. The average period as well as the plot scales were completely
variable. Various detectors outputs could be grouped together and ratios
of various detector outputs could be plotted. Input to the system was the
edited tapes produced by the Si EDIT program.
7. S2 RATE
The S2 RATE program produced a listing of the raw counts and
observed counting rates for the IMP-5 S2 experiment. The listing was
non-fill points. The program was written by G. Pitt and later modified
by C. Wittnebert in November, 1969.
III. List of Publications Reporting Results From IMP-4 and 5 Satellites
Alvarez, H. F. Haddock, and R.P. Lin, Evidence for electron excitation
of type III radio burst emission, Solar Phys., 26, 468, 1972.
Anderson, K.A., Electrons and protons in long-lived streams of energetic
solar particles, Solar Physics, 6, 111, 1969.
Anderson, K.A., S.R. Kane and R.P. Lin, Fast electrons in solar flares,
International Seminar on the Problem of Cosmic Ray Generation on
the sun, Leningrad, USSR, December, 1970, (SSL Series 12, Issue 7).
Anderson, K.A. and R.P. Lin, Information on the University of California
experiments in the Explorer 33 and 35 satellites (Lunar Anchored
IMP's) and the Explorer 34 and 41 satellites (IMP's 4 and 5), UCB
SSL Technical Report, Series 11, Issue 89, 1970.
Anderson, K. A., Particle Acceleration by Shock Waves in the Solar System,
to be published in Proceedings of the Leningrad Seminar on Generality
of Particle Acceleration, Leningrad, USSR, August, 1972.
Kane, S.R. and R.P. Lin, Location of the electron acceleration region
in solar flares, Solar Phys., 23, 457, 1972.
Lin, R.P., The emission and propagation of ~40 keV solar electrons,
Proc. XI Int. Conf. on Cosmic Rays, Budapest, 1969 Acta Physica
Acad. Sci.. Hungaricae, 29, Suppl. 2, 669, 1970.
Lin, R.P., Observations of scatter-free propagation of ~40 keV solar
electrons in the interplanetary medium, J. Geophys. Res., 75,
2583, 1970.
Lin, R.P., The emission and propagation of N40 keV solar flare electrons
I. Relationship of ~ 40 keV electron to energetic proton and rela-
tivistic electron emission by the sun, Solar Phys. 12, 266, 1970.
Lin, R.P., The emission and propagation of ~ 40 keV solar flare electrons
II. The electron emission structure of large active regions, Solar
Phys. 15, 453, 1970.
Lin, R.P. and H.S. Hudson, 10-100 keV electron acceleration and emission
from solar flares, Solar Phys., 17, 412, 1971.
Lin, R.P., Acceleration of 10-100 keV electrons in solar flares, International
Seminar on the Acceleration of Particles in Near-Earth and Inter-
planetary Space, Galaxy and Metagalaxy, Leningrad, USSR, July
13-15, 1971 (SSL Series 12, Issue 63).
Lin, R.P., Energy spectra of solar flare electrons, Proc. 1971 XII
International Cosmic Ray Conference, Hobart, Tasmania, Australia,
August, 1971.
Lin, R.P., Acceleration of electrons in Solar Flares, to be published in
the Proceedings of the Solar Terrestrial Relations Conference,
Calgary, Canada, August 28-September 1, 1972.
Lin, R.P., The relationship of solar flare electrons to the flare flash
phase and type III radio bursts, to be published in the "High Energy
Phenomena on the Sun, " the Proceedings of the Symposium on
High Energy Phenomena on the Sun held at Goddard Space Flight
Center, September, 1972.
Lindgren, S.T., The solar particle events of May 23 and May 28, 1967,
Solar Phys., 4, 338, 1968.
Palmer, I. D. and R.P. Lin, The position and size of radio sources
associated with solar electron events, to be published in "High
Energy Phenomena on the Sun, " the Proceedings of the Symposium
on High Energy Phenomena on the Sun held at Goddard Space Flight
Center, September, 1972.
Palmer, I.D. and R.P. Lin, The coronal site of a type III burst as a
source of interplanetary electrons, Proc. Astron. Soc., Australia,
2, 101, 1972.
IV. Papers Presented at Scientific Meetings Reporting Results From
the IMP-4 and 5 Satellites
Lin, R.P., Fluxes of ~40 keV electrons associated with solar active
regions, AGU, Washington, D.C., April, 1969.
Roelof, E. C. and R.P. Lin, Coronal storage and interplanetary propagation
of low energy solar particles, AGU, San Francisco, California,
December, 1969.
Lin, R.P., Observations of solar flare electrons, invited review paper,
AGU, San Francisco, California, December 1970.
Lin, R.P., J.R. Wang, and L.A. Fisk, Scatter-free electron propagation
in the interplanetary medium, AGU, San Francisco, California,
December, 1972.
McGuire, R.E., K.A. Anderson, L.M. Chase, R.P. Lin, and J.E. McCoy,
Particle observations during the passage of the interplanetary shock
of May 15, 1972, AGU, San Francisco, California, December, 1972.
Wang, J.R., L.A. Fisk and R.P. Lin, Observations of the scatter-free
solar-flare electrons in the energy range 20-1000 keV, 12th
International Conference on Cosmic Rays, Hobart, Tasmania,
Australia, August, 1971.
Lin, R.P., Energy spectra of solar flare electrons, 12th International
Conference on Cosmic Rays, Hobart, Tasmania, Australia,
August, 1971.
Lin, R.P. and K.A. Anderson, Solar electron events in mid-1967, AGU,
San Francisco, California, December, 1968.
Lin, R.P., The emission and propagation of ~ 40 keV solar electrons,
11th International Conference on Cosmic Rays, Budapest, Hungary,
1969.
Anderson, K.A., Low energy electrons and protons from the sun, lth
International Conference on Cosmic Rays, Budapest, Hungary, 1969.


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