SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 351, 330-340 (1999)

Next Section Table of Contents

On the origin of TeV radiation of SN 1006

F.A. Aharonian 1 and A.M. Atoyan 1,2

1 Max-Planck-Institut für Kernphysik, Postfach 103980, 69029 Heidelberg, Germany
2 Yerevan Physics Institute, Alikhanian Br. 2, 375036 Yerevan, Armenia

Received 26 February 1999 / Accepted 9 September 1999

Abstract

We discuss the link between the nonthermal X-radiation and TeV [FORMULA]-ray emission from SN 1006, and study the capabilities of both electronic and nucleonic models for explanation of the TeV flux observed from the northeast rim of SN 1006. We show that the interpretation of the TeV radiation by the inverse Compton scattering of electrons on 2.7 K cosmic microwave background radiation is possible, however due to the escape of high energy electrons, the [FORMULA]-ray emission should be significantly contributed not only from the rim, but also from the inner parts of the remnant. This implies an angular size of the TeV [FORMULA]-ray emission larger than the size of the nonthermal X-radiation. In this scenario the magnetic field in the rim should not exceed [FORMULA]. Then, in order to allow acceleration of particles well beyond 10 TeV the shock speed should be high, [FORMULA]. The latter condition gives preference to a large distance to the source, [FORMULA] or so which is in the limits of distances currently discussed in the literature. On the other hand, a larger magnetic field of order [FORMULA] and smaller shock speeds (and therefore a small distance to the source of about 1 kpc) are not excluded. In that case the observed TeV radiation can be explained by shock accelerated protons in the rim through production and subsequent decay of [FORMULA]-mesons. Contrary to IC radiation, the [FORMULA]-decay [FORMULA]-ray source coincides essentially with the rim, and therefore it could be recognized by a relatively compact angular width. Both the electronic and nucleonic models require high efficiency of particle acceleration close to the Bohm limit, and large total energy in accelerated particles at the level of respectively [FORMULA] and [FORMULA] of the kinetic energy of explosion of SN 1006. We discuss observational possibilities to distinguish between electronic and nucleonic origins of [FORMULA]-radiation.

Key words: radiation mechanisms: non-thermal – stars: supernovae: individual: SN 1006 – gamma rays: theory – X-rays: stars

Send offprint requests to: F.A. Aharonian (Felix.Aharonian@mpi-hd.mpg.de)

SIMBAD Objects

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 1999

Online publication: November 2, 1999
helpdesk.link@springer.de