Hostname: page-component-cc8bf7c57-77pjf Total loading time: 0 Render date: 2024-12-12T07:58:40.431Z Has data issue: false hasContentIssue false

Detection of TeV Gamma Rays from SN1006

Published online by Cambridge University Press:  25 May 2016

Toru Tanimori*
Affiliation:
Department of Physics, Tokyo Institute of Technology Ohokayama, Meguro, Tokyo 152, Japan

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In spite of the recent progress of high energy gamma-ray astronomy, there still remains quite unclear and important problem about the origin of cosmic rays. Supernova remnants (SNRs) are the favoured site for cosmic rays up to 1016 eV, as they satisfy the requirements such as an energy input rate. But direct supporting evidence is sparse. Recently intense non-thermal X-ray emission from the rims of the Type Ia SNR SN1006 (G327.6+14.6) has been observed by ASCA (Koyama et al. 1995)and ROSAT (Willingale et al. 1996), which is considered, by attributing the emission to synchrotron radiation, to be strong evidence of shock acceleration of high energy electrons up to ~100 TeV. If so, TeV gamma rays would also be expected from inverse Compton scattering (IC) of low energy photons (mostly attributable to the 2.7 K cosmic background photons) by these electrons. By assuming the magnetic field strength (B) in the emission region of the SNR, several theorists (Pohl 1996; Mastichiadis 1996; Mastichiadis & de Jager 1996; Yoshida & Yanagita 1997) calculated the expected spectra of TeV gamma rays using the observed radio/X-ray spectra. Observation of TeV gamma rays would thus provide not only the further direct evidence of the existence of very high energy electrons but also the another important information such as the strength of the magnetic field and diffusion coefficient of the shock acceleration. With this motivation, SN1006 was observed by the CANGAROO imaging air Cerenkov telescope in 1996 March and June, also 1997 March and April.

Type
Session 3: Diagnostics of High Gravity Objects with X- and Gamma Rays
Copyright
Copyright © Kluwer 1998 

References

Hara, T. et al. (1993), Nuc. Inst. Meth. Phys. Res. A , 332, 300309 CrossRefGoogle Scholar
Kifune, T. et al. (1995), Astrophys. J. , 438, L91L94 CrossRefGoogle Scholar
Koyama, K. et al. (1995), Nature , 378, 255258 CrossRefGoogle Scholar
Mastichiadis, A. (1996), Astr. Astrophys. , 305, L53L56 Google Scholar
Mastichiadis, A. & de Jager, O.C. (1996), Astr. Astrophys. , 311, L5L8 Google Scholar
Patterson, J. R., & Kifune, T. (1992), Australian and New Zealand Physicist , 29, 5862 Google Scholar
Pohl, M. (1996), Astr. Astrophys. , 307, 57395 Google Scholar
Reynolds, S.P. & Ellison, D.C. (1991), Proc. 22nd Int. Cosmic ray Conf. , 2 404407 Google Scholar
Tanimori, T. et al. (1997), IAU Circ. No. 6706 Google Scholar
Tanimori, T. et al. (1998), Astrophys. J. , in press Google Scholar
Yoshida, T. & Yanagita, S. (1997), Proc. 2nd INTEGRAL Workshop , ESA SP382 8588 Google Scholar
Weekes, T.C. et al. (1989), Astrophys. J. , 342, 379395 CrossRefGoogle Scholar
Willingale, R. et al. (1996) Mon. Not. R. astr. Soc. , 278, 749762 CrossRefGoogle Scholar