Magnetic field in supernova remnant SN 1987A
arXiv:astro-ph/0608586 · doi:10.1086/508615
Abstract
A nonlinear kinetic theory of cosmic ray (CR) acceleration in supernova remnants is employed to investigate the properties of the remnant SN 1987A. It is shown that a large downstream magnetic field ~10 mG is required to fit the existing observational data. Such a strong field together with the strong shock modification due to CR backreaction provides the steep and concave radioemission spectrum and considerable synchrotron cooling of high energy electrons which diminish their X-ray synchrotron flux below the observed Chandra flux which has to be considered as an upper limit for nonthermal X-ray emission. The expected gamma-ray energy flux at TeV-energies at the current epoch is 2x10^{-13} erg/(cm^2 s).
12 pages, 4 figures, accepted for publication in ApJ Letters
References in corpus (1)
Cited by in corpus (5)
- Spectral and morphological analysis of the remnant of Supernova 1987A with ALMA & ATCA
- Cosmic Ray Acceleration by Supernova Shocks
- Multi-dimensional simulations of the expanding supernova remnant of SN 1987A
- Thermal Emission and Radioactive Lines, but No Pulsar, in the Broadband X-Ray Spectrum of Supernova 1987A
- Expected gamma-ray emission of supernova remnant SN 1987A