Optical radiation and radio emission accompanying cosmic gamma bursts

Details Optical radiation and radio emission accompanying cosmic gamma bursts Optical radiation and radio emission accompanying cosmic gamma bursts

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986rpspr...6...85v&link_type=abstract

In its USSR Report: Space (JPRS-USP-86-001) p 85-86 (SEE N86-20178 10-88) Transl. into ENGLISH from Pisma v Astronomicheskiy

Astronomy and Astrophysics

Astronomy

Antenna Arrays, Gamma Ray Bursts, Light (Visible Radiation), Radiation Detectors, Radio Emission, Cerenkov Radiation, Earth Atmosphere, Electrons, Relativistic Particles, Spacecraft Instruments

Scientific paper

In order to register cosmic gamma radiation with an energy 10 GeV and fluxes 0.0000000001 quantum/square centimeters times s it is necessary to have greater areas of detectors than those now present on spacecraft. C. Castagnoli, et al., proposed that gamma quanta with energies 0.00001 GeV be registered on the basis of records of Cerenkov flares from relativistic electrons of extensive atmospheric showers caused in the Earth's upper atmosphere by primary gamma quanta using large solar antenna arrays at nighttime. With that proposal taken into account, the authors have evaluated the intensity of the light flashes excited in the atmosphere by gamma bursts. Calculations are given showing that the maximum intensity of atmospheric glow in the band lambda = 3914 A will be Imax = 0.000001 minus 0.001 erg/square centimeters times s. In the case of the powerful gamma burst of 5 March 1979 Imax equals 2 times 0.000001 erg/square centimeters. It is concluded that light flashes of this intensity can be registered using the large solar antenna arrays which it is proposed to be used for measuring the Cerenkov radiation (with an intensity 0.0000001 erg/square centimeters times s) from high-energy gamma quanta. The intensity of the light gamma flashes excited in the atmosphere by gamma bursts (0.01 minus 10 MeV) in order of magnitude coincides with the intensity of the Cerenkov radiation excited by electron showers from gamma quanta (10 minus 0.001 GeV) so that these flares must be taken into account in the registry of high-energy gamma quanta. Since there is a common nature of the mechanism for generation of optical and radio signals, they can be used together in the registry of cosmic gamma bursts.

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