A Gamma Ray Monitor for the OSO-7 Spacecraft

Higbie, P. R.; Chupp, E. L.; Forrest, D. J.; Gleske, I. U.

doi:10.1109/tns.1972.4326565

Cited by 9 publications

(2 citation statements)

References 2 publications

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“…The gamma ray detector on the OSO-7 satellite has been described in detail by Higbie et al (1972). Briefly, the detector consisted of a 7.6 cm x 7.6 cm Na I (T1) crystal surrounded by a cup-shaped active shield of Cs I (Na) and was located in the spinning wheel section of the spacecraft.…”

Section: Observationsmentioning

confidence: 99%

Observations of solar gamma ray continuum between 360 keV and 7 MeV on August 4, 1972

et al. 1975

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Measurements were made of the time-averaged gamma ray energy loss spectrum in the energy range 360 keV to 7 MeV by the gamma ray detector on the OSO-7 satellite during the 3B flare on August 4, 1972. The differential photon spectrum unfolded from this spectrum after subtracting the background spectrum and contributions from gamma ray lines is best described by a power law with spectral index of 3.4d_0.3 between 360-700 keV and by an exponential law of the form exp (--E/Eo) with E0=l.0• MeV above 700 keV. It is suggested that this spectrum is due to nonthermal electron bremsstrahlung from a population of electrons, with a strong break in the spectrum at 2 MeV. Since the observational data indicates that the matter number density must be n~ ~> 5 • 101~ cm -a in the production region, the number of electrons above 100 keV required to explain the results is ~< 2 x 10 a4.

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Section: Observationsmentioning

confidence: 99%

Observations of solar gamma ray continuum between 360 keV and 7 MeV on August 4, 1972

et al. 1975

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“…Originally, X ray data from the University of New Hampshire (UNH) instrumentation aboard the Oso 7 spacecraft were used. The X ray data came from a small detector covering the 7.5-to 120-keV range in four channels [Higbie et al, 1972]. (The primary objective of the UNH experiment was the detection and study of 0.3-to 10-MeV gramma rays produced by relativistic electrons or nuclear reactions.)…”

Section: H^rd X Ray and Optical Considerationsmentioning

confidence: 99%

Solar bursts at λ = 2 cm on July 31, 1972

Castelli¹,

Guidice²,

Forrest³

et al. 1974

J. Geophys. Res.

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On July 31, 1972, McMath plage 11976 was the site of many moderate‐intensity solar radio bursts with unusual radio spectra, emission being limited to only short‐centimeter (and possibly millimeter) wavelengths. This same plage region was responsible for the historic solar geophysical events of early August 1972. Unlike most microwave bursts, which have their spectral maximums (ƒmax) in the 2‐ to 10‐GHz range, these July 31 bursts had their ƒmax at ≳15 GHz with extremely steep slopes (≥5) on the low‐frequency side of ƒmax and cutoff frequencies generally at ≳10 GHz. Most of the July 31 bursts observed were impulsive, with time profiles similar to those of the X ray emission in the 7.5‐ to 15‐keV and 15‐ to 30‐keV ranges. From the radio spectral characteristics a number of concepts concerning conditions within the burst region are considered and found to present difficulties. Some general conclusions on the burst region properties are reached.

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