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Radiation Bursts from a Presupernova Collapsar

Published online by Cambridge University Press:  19 September 2016

Volodymyr Kryvdyk
Volodymyr Kryvdyk*
Affiliation:
Kyiv National University, av. Glushkova 6, Kyiv 03022, Ukraine;kryvdyk@mail.univ.kiev.ua

Summary

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The radiation from the magnetic presupernova star is calculated. This radiation will generate when the magnetosphere of presupernova star compresses during collapse and its magnetic field increases considerably. The variable magnetic field will accelerate the charged particle, which generate radiation when moving in the magnetic field. The particles dynamics and their non-thermal emission in the magnetospheres of presupernova collapsing star with initial dipole magnetic fields and a certain initial energy distribution of charged particles in a magnetosphere are considered. The radiation flux depend on the distance to the star, its magnetic field, and the particle spectrum in the magnetosphere. This flux can be observed by means of modern instruments in broad band (from radio waves to gamma rays). The radiation flux grows with decreasing stellar radius and frequency and can be observed in the form of radiation bursts with duration equal to the stellar collapse time.

Type
Part III Supernovae: Progenitors/Remnants
Information
International Astronomical Union Colloquium , Volume 192: Cosmic Explosions , 2005 , pp. 215 - 218
Copyright
Copyright © Springer-Verlag 2005

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