Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment
LEI Hai-Dong1, WANG Jiu-Zhou2, LÜ Jing2, ZOU Yuan-Chuan2**
1Department of Physics and Electronics, Jianghan University, Wuhan 430056 2School of Physics, Huazhong University of Science and Technology, Wuhan 430074
Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment
LEI Hai-Dong1, WANG Jiu-Zhou2, LÜ Jing2, ZOU Yuan-Chuan2**
1Department of Physics and Electronics, Jianghan University, Wuhan 430056 2School of Physics, Huazhong University of Science and Technology, Wuhan 430074
摘要We investigate the shallow decay phase of an early x-ray afterglow in gamma-ray bursts discovered by Swift, and suggest that both the shallow decay phase and the normal phase are from external shock in a wind environment, while the transferring time is the deceleration time. We apply this model to GRBs 050319 and 081008, and find that they can be explained by choosing a proper set of parameters.
Abstract:We investigate the shallow decay phase of an early x-ray afterglow in gamma-ray bursts discovered by Swift, and suggest that both the shallow decay phase and the normal phase are from external shock in a wind environment, while the transferring time is the deceleration time. We apply this model to GRBs 050319 and 081008, and find that they can be explained by choosing a proper set of parameters.
LEI Hai-Dong;WANG Jiu-Zhou;LÜJing;ZOU Yuan-Chuan**
. Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment[J]. 中国物理快报, 2011, 28(12): 129801-129801.
LEI Hai-Dong, WANG Jiu-Zhou, LÜ, Jing, ZOU Yuan-Chuan**
. Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment. Chin. Phys. Lett., 2011, 28(12): 129801-129801.
[1] Nousek J A et al 2006 Astrophys. J. 642 389
[2] O'Brien P T et al 2006 Astrophys. J. 647 1213
[3] Zhang B et al 2006 Astrophys. J. 642 354
[4] Toma K, Ioka K, Yamazaki R and Nakamura T 2006 Astrophys. J. 640 L139
[5] Ioka K, Toma K, Yamazaki T and Nakamura T 2006 Astron. & Astrophys. 458 7
[6] Wu X F et al 2006 36th COSPAR Sci. Ass. #731(arXiv:astro-ph/0512555)
[7] Zou Y C and Dai Z G 2006 Chin. J. Astron. Astrophys. 6 551
[8] Zou Y C, Dai Z G and Xu D 2006 Astrophys. J. 646 1098
[9] Xu M and Huang Y F 2010 Astron. Astrophys. 523 5
[10] Fan Y Z and Piran T 2006 Mon. Not. R. Astron. Soc. 369 197
[11] Kong S W, Wong A Y L, Huang Y F and Cheng K S 2010 Mon. Not. R. Astron. Soc. 402 409
[12] Ghisellini G, Ghirlanda G, Nava L and Firmani C 2007 Astrophys. J. 658 L75
[13] Yamazaki R 2009 Astrophys. J. 690 L118
[14] Liang E W, Lv H J, Hou S J, Zhang B B and Zhang B 2009 Astrophys. J. 707 328
[15] Dai Z G and Lu T 1998 Mon. Not. R. Astron. Soc. 298 87
[16] Chevalier R A and Li Z Y 2000 Astrophys. J. 536 195
[17] Fan Y Z and Wei D M 2005 Mon. Not. R. Astron. Soc. 364 L42
[18] Xue R R, Fan Y Z and Wei D M 2009 Astron. & Astrophys. 498 671
[19] Shen R F and Matzner C D 2011 arXiv:1109.3453v2 [astro-ph]
[20] Zhang B, Koabyashi S, and Mészáros P 2003 Astrophys. J. 595 950
[21] Zou Y C, Wu X F and Dai Z G 2005 Mon. Not. R. Astron. Soc. 363 93
[22] Rees M J and Mészáros P 1992 Mon. Not. R. Astron. Soc. 258 41p
[23] Sari R, Piran T and Narayan R 1998 Astrophys. J. 497 L17
[24] Cusumano G et al 2006 Astrophys. J. 639 316
[25] Yuan F et al 2010 Astrophys. J. 711 870
[26] Krimm H A et al 2007 Astrophys. J. 665 554
[27] Liang E W, Zhang B B and Zhang B 2007 Mon. Not. R. Astron. Soc. 670 565
[28] Panaitescu A 2006 Mon. Not. R. Astron. Soc. 369 2059
[29] Zhang B 2006 Advances in Space Research 40 1186
[30] Perri M et al 2005 Astron. Astrophys. 442 L1