A NEW CLASSIFICATION METHOD FOR GAMMA-RAY BURSTS
A NEW CLASSIFICATION METHOD FOR GAMMA-RAY BURSTS
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伽马射线暴的新分类方法
DOI：
10.1088/0004-637x/725/2/1965
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发表时间：
2010-01
影响因子：
4.9
通讯作者：
Zhang, Bin-Bin
中科院分区：
文献类型：
--
作者：
Lue, Hou-Jun;Zhang, Bing;Liang, En-Wei;Zhang, Bin-Bin
最近的Swift观测表明，传统的长与短伽马射线暴（GRB）分类方案并不总是将GRB与两种物理动机模型类型相关联，即，II型（大质量星星起源）与I型（致密星星起源）。通过引入新的参数ε = Eγ，iso，52/E5/3 p，z，2，提出了一种新的伽玛暴唯象分类方法，其中Eγ，iso是各向同性伽玛射线能量（单位为1052 erg），Ep，z是宇宙静止框架谱峰能量（单位为100 keV）.对于那些具有“扩展发射”的短伽玛暴，这两个量仅针对短/硬尖峰定义。利用目前完整的具有红移和Ep测量的伽玛暴样本，ε参数显示出明显的双峰分布，分离度为ε = 0.03。高ε区包括典型的高亮度长暴、一些高z“静止-短帧”暴（如GRB 090423和GRB 080913）以及一些高z短暴（如GRB 090426）。根据文献中的其他观测性质，所有这些伽玛暴都被认为是II型起源的。所有被认为是I型起源的伽玛暴都聚集在低ε区。它们可以通过一个附加的T90判据与附近的一些低光度长伽玛暴（3σ）分离，即，T90，z 15 s在Swift/BAT波段。我们认为，这种新的分类方案可以更好地匹配物理驱动的II/I型分类方案。
Recent Swift observations suggest that the traditional long versus short gamma-ray burst (GRB) classification scheme does not always associate GRBs to the two physically motivated model types, i.e., Type II (massive star origin) versus Type I (compact star origin). We propose a new phenomenological classification method of GRBs by introducing a new parameter ε = Eγ,iso,52/E5/3p,z,2, where Eγ,iso is the isotropic gamma-ray energy (in units of 1052 erg) and Ep,z is the cosmic rest-frame spectral peak energy (in units of 100 keV). For those short GRBs with “extended emission,” both quantities are defined for the short/hard spike only. With the current complete sample of GRBs with redshift and Ep measurements, the ε parameter shows a clear bimodal distribution with a separation at ε ∼ 0.03. The high-ε region encloses the typical long GRBs with high luminosity, some high-z “rest-frame-short” GRBs (such as GRB 090423 and GRB 080913), as well as some high-z short GRBs (such as GRB 090426). All these GRBs have been claimed to be of Type II origin based on other observational properties in the literature. All the GRBs that are argued to be of Type I origin are found to be clustered in the low-ε region. They can be separated from some nearby low-luminosity long GRBs (in 3σ) by an additional T90 criterion, i.e., T90,z ≲ 5 s in the Swift/BAT band. We suggest that this new classification scheme can better match the physically motivated Type II/I classification scheme.
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GRB 090423：标志着 z=8.2 处大质量恒星的死亡
DOI：
10.1007/s11433-010-0027-z
发表时间：
2009-06
期刊：
Science in China G: Physics and Astronomy
影响因子：
--
作者：
Zhang Shuangnan;Lin Lin;Liang Enwei
通讯作者：
Liang Enwei
DOI：
10.1086/506271
发表时间：
2006-03
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
B. Cobb;C. Bailyn;P. G. V. Dokkum;Priya Natarajan
通讯作者：
B. Cobb;C. Bailyn;P. G. V. Dokkum;Priya Natarajan
影响因子：
64.8
作者：
A. Soderberg;S. Kulkarni;Edo Berger;D. Fox;Masao Sako;D. Frail;A. Gal-yam;D. Moon;S. Cenko;S. Yost;M. M. Phillips-M.;S. E. Persson;W. Freedman;P. Wyatt;R. Jayawardhana;D. Paulson
通讯作者：
A. Soderberg;S. Kulkarni;Edo Berger;D. Fox;Masao Sako;D. Frail;A. Gal-yam;D. Moon;S. Cenko;S. Yost;M. M. Phillips-M.;S. E. Persson;W. Freedman;P. Wyatt;R. Jayawardhana;D. Paulson
DOI：
10.1088/0004-637x/698/2/1620
发表时间：
2008-02
期刊：
The Astrophysical Journal
影响因子：
--
作者：
J. Graham;A. Fruchter;A. Levan;A. Melandri;L. Kewley;E. Levesque;M. Nysewander;N. Tanvir;T. Dahlén;D. Bersier;K. Wiersema;D. Bonfield;A. Martínez-Sansigre
通讯作者：
J. Graham;A. Fruchter;A. Levan;A. Melandri;L. Kewley;E. Levesque;M. Nysewander;N. Tanvir;T. Dahlén;D. Bersier;K. Wiersema;D. Bonfield;A. Martínez-Sansigre
影响因子：
64.8
作者：
Della Valle, M.;Chincarini, G.;Stella, L.
通讯作者：
Stella, L.