| GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS |
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Nonthermal Emission of Tycho's Supernova Remnant |
| TANG Yun-Yong, FANG Jun, ZHANG Li**
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Department of Physics, Yunnan University, Kunming 650091
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| Cite this article: |
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TANG Yun-Yong, FANG Jun, ZHANG Li 2011 Chin. Phys. Lett. 28 109501 |
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Abstract The time-dependent non-thermal particle and photon spectra are reproduced for a Type Ia SNR Tycho with radio, x-ray, GeV and TeV emission within the framework of the diffusive shock acceleration of the non-thermal particles. TeV photons can come from the inverse Compton scattering of relativistic electrons and from the π0−decay process in proton-proton interaction. The results show that (1) the hadronic case can model the observed multiwavelength spectrum well and, peculiarly, the π0-decay process appears to be necessary to explain the GeV emission; and (2) magnetic field amplification is vital in the SNR.
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| Keywords:
95.30.Gv
98.58.Db
98.58.Mj
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Received: 13 June 2011
Published: 28 September 2011
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| PACS: |
95.30.Gv
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(Radiation mechanisms; polarization)
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98.58.Db
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(Molecular clouds, H2 clouds, dense clouds, and dark clouds)
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98.58.Mj
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(Supernova remnants)
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[1] Dickel J R, van Breugel W J M and Strom R G 1991 Astron. J. 101 2151
[2] Stroman W and Pohl M 2009 Astrophys. J. 696 1864
[3] Kothes R, Fedotov K, Foster T J and Uyaniker B 2006 Astron. Astrophys. 457 1081
[4] Hwang U, Petre R, Szymkowiak A E and Holt S S 2002 J. Astrophys. Astron. 23 81
[5] Bamba A, et al 2005 Astrophys. J. 621 793
[6] Warren J S et al 2005 Astrophys. J. 634 376
[7] Katsuda S, Petre R, Hughes J P, Hwang U, Yamaguchi H, Hayato A, Mori K and Tsunemi H 2010 Astrophys. J. 709 1387
[8] Tamagawa T et al 2009 Publ. Astron. Soc. Jpn. 61 167
[9] Giordano F et al 2010 Proceedings of the 25th Texas Symposium (Heidelberg, Germany)
[10] Naumann-Godo M at al 2011 Poster at the 3rd Fermi Symposium (Rome, Italy)
[11] Acciari V A et al 2011 Astrophys. J. 730 L20
[12] Reynoso E M et al 1999 Astron. J. 117 1827
[13] Lee J, Koo B, and Tatematsu K 2004 Astrophys. J. 605 L113
[14] Cai Z, Yang J and Lu D 2009 Chin. J. Astron. Astrophys. 33 393
[15] Tian W W, and Leahy D A 2011 Astrophys. J. 729 L15
[16] Krause O et al 2008 Nature 456 617
[17] Hayato A 2010 Astrophys. J. 725 894
[18] Zhang L and Fang J 2007 Astrophys. J. 666 247
[19] Fang J and Zhang L 2008 Mon. Not. R. Astron. Soc. 384 1119
[20] Caprioli D, Amato E and Blasi P 2010 Astropart. Phys. 33 307
[21] Kamae T et al 2006 Astrophys. J. 647 692
[22] Reynolds S P and Ellison D C 1992 Astrophys. J. 399 L75
[23] Morlino G and Caprioli D 2011 preprint arXiv:1105.6342
[24] Berezhko E G and Völk H J 1997 Astropart. Phys. 7 183
[25] Ellison D C, Berezhko E G and Baring M G 2000 Astrophys. J. 540 292
[26] Amato E and Blasi P 2006 Mon. Not. R. Astron. Soc. 371 1251
[27] Völk H J, Berezhko E G and Ksenofontov L T 2008 Astron. Astrophys. 483 529
[28] Blandford R D and Eichler D 1987 Phys. Rep. 154 1
[29] Ballet J 2006 Adv. Space. Res. 37 1902
[30] Marcowith A and Casse F 2010 Astron. Astrophys. 515 id.A90
[31] Caprioli D, Blasi P, Amato E and Vietri M 2008 Astrophys. J. 679 L139 |
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