The high energy gamma-ray emission expected from Tycho's supernova remnant

Details The high energy gamma-ray emission expected from Tycho's supernova remnant The high energy gamma-ray emission expected from Tycho's supernova remnant

2002-10-08

arxiv.org/abs/astro-ph/0210176v1

Astron.Astrophys. 396 (2002) 649-656

Astronomy and Astrophysics

Astrophysics

8 pages, 6 figures. Accepted in Astronomy and Astrophyics

Scientific paper

10.1051/0004-6361:20021407

A nonlinear kinetic model of cosmic ray (CR) acceleration in supernova remnants (SNRs) is used to describe the properties of Tycho's SNR. Observations of the expansion characteristics and of the nonthermal radio and X-ray emission spectra, assumed to be of synchrotron origin, are used to constrain the overall dynamical evolution and the particle acceleration parameters of the system, in addition to what is known from independent estimates of the distance and thermal X-ray observations. It is shown that a very efficient production of nuclear cosmic rays, leading to strong shock modification, and a large downstream magnetic field strength B_d approx 240muG are required to reproduce the observed synchrotron emission from radio to X-ray frequencies. This field strength is still well within the upper bound for the effective magnetic field, consistent with the acceleration process. The pi^0-decay gamma-ray flux turns out to be somewhat greater than the inverse Compton (IC) flux off the Cosmic Microwave Background at energies below 1 TeV, dominating it strongly at 10 TeV. The predicted TeV gamma-ray flux is consistent with but close to the very low upper limit recently obtained by HEGRA. A future detection at E_gamma ~ 10 TeV would clearly indicate hadronic emission.

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