伽玛暴(Gamma-Ray Burst)笔记。记录有关伽玛暴的新文章,另外也包括看的老文章、自己的想法、以及跟天文相关的一些东西。 Feel free to leave me a message by comments or by email.

星期二, 四月 19, 2011

Levan 2011 GRB 110328A的观测

主要内容:

全名GRB110328A/Swift J164449.3+573451, 红移约0.5,可能不是伽马暴,但又比AGN的峰值能量高很多。

说可能是一个被星系级黑洞吞噬的恒星。
新闻参考:http://bzhang.lamost.org/website/archives/grb110328a_nasa/

精彩摘抄:

Add caption

x射线光变,看起来实在不像伽马暴

文章信息:

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· arXiv e-print (arXiv:1104.3356)
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Title:
An extremely luminous panchromatic outburst from the nucleus of a distant galaxy
Authors:
Levan, A. J.; Tanvir, N. R.; Cenko, S. B.; Perley, D. A.; Wiersema, K.; Bloom, J. S.; Fruchter, A. S.; de Ugarte Postigo, A.; O'Brien, P. T.; Butler, N.; van der Horst, A. J.; Leloudas, G.; Morgan, A. N.; Misra, K.; Bower, G.; Farihi, J.; Tunnicliffe, R. L.; Modjaz, M.; Silverman, J. M.; Hjorth, J.; Thoene, C.; Cucchiara, A.; Castro Ceron, J. M.; Castro-Tirado, A.; Arnold, J. A.; Bremer, M.; Brodie, J. P.; Carroll, T.; Cooper, M. C.; Curran, P. A.; Cutri, R. M.; Ehle, J.; Forbes, D.; Fynbo, J.; Gorosabel, J.; Graham, J.; Guizy, S.; Hoffman, D. I.; Jakobsson, P.; Kamble, A.; Kerr, T.; Kasliwal, M. M.; Kouveliotou, C.; Kocesvki, D.; Law, N. M.; Nugent, P. E.; Ofek, E. O.; Poznanski, D.; Quimby, R. M.; Rol, E.; Romanowsky, A. J.; Sanchez-Ramirez, R.; Schulze, S.; Singh, N.; Starling, R. L. C.; Strom, R. G.; Wheatley, P. J.; Wijers, R. A. M. J.; Winters, J. M.; Wold, T.; Xu, D.
Publication:
eprint arXiv:1104.3356
Publication Date:
04/2011
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Bibliographic Code:
2011arXiv1104.3356L

Abstract

Variable X-ray and gamma-ray emission is characteristic of the most extreme physical processes in the Universe, and studying the sources of these energetic photons has been a major driver in astronomy for the past 50 years. Here we present multiwavelength observations of a unique gamma-ray selected transient, discovered by Swift, which was accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z=0.3534. Its high-energy emission has lasted much longer than any gamma-ray burst, while its peak luminosity was about 100 times higher than the brightest active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a new, rare mechanism associated with a massive black hole in the nucleus of a galaxy.

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Luchkov 2011 有些伽马暴可能是来自银河系内恒星的闪耀

主要内容:
通过暴的坐标和恒星的坐标对比,发现有四个位置对得上。而他们计算的巧合的可能性只有4E-5.

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Title:
Stellar Sources of Gamma-ray Bursts
Authors:
Luchkov, B. I.
Publication:
eprint arXiv:1104.3351
Publication Date:
04/2011
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Galaxy Astrophysics
Comment:
2 pages
Bibliographic Code:
2011arXiv1104.3351L

Abstract

Correlation analysis of Swift gamma-ray burst coordinates and nearby star locations (catalog Gliese) reveals 4 coincidences with good angular accuracy. The random probability is 4\times 10^{-5}, so evidencing that coincident stars are indeed gamma-ray burst sources. Some additional search of stellar gamma-ray bursts is discussed.
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星期六, 四月 02, 2011

Collazzi 2011 E_p的值还是有很大的误差

主要内容:


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Title:
The Total Errors In Measuring Epeak for Gamma-Ray Bursts
Authors:
Collazzi, Andrew C.; Schaefer, Bradley E.; Moree, Jeremy A.
Publication:
eprint arXiv:1101.1285
Publication Date:
01/2011
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Comment:
25 pages, 2 figures, ApJ accepted
Bibliographic Code:
2011arXiv1101.1285C

Abstract

While Epeak has been extensively used in the past, for example with luminosity indicators, it has not been thoroughly examined for possible sources of scatter. In the literature, the reported error bars for Epeak are the simple Poisson statistical errors. Additional uncertainties arise due to the choices made by analysts in determining Epeak (e.g., the start and stop times of integration), imperfect knowledge of the response of the detector, different energy ranges for various detectors, and differences in models used to fit the spectra. We examine the size of these individual sources of scatter by comparing many independent pairs of published Epeak values for the same bursts. Indeed, the observed scatter in multiple reports of the same burst (often with the same data) is greatly larger than the published statistical error bars. We measure that the one-sigma uncertainty associated with the analyst's choices is 28%, i.e., 0.12 in Log10(Epeak), with the resultant errors always being present. The errors associated with the detector response are negligibly small. The variations caused by commonly-used alternative definitions of Epeak (such as present in all papers and in all compiled burst lists) is typically 23%-46%, although this varies substantially with the application. The implications of this are: (1) Even the very best measured Epeak values will have systematic uncertainties of 28%. (2) Thus, GRBs have a limitation in accuracy for a single event, with this being reducible by averaging many bursts. (3) The typical one-sigma total uncertainty for collections of bursts is 55%. (4) We also find that the width of the distribution for Epeak in the burst frame must be near zero, implying that some mechanism must exist to thermostat GRBs. (5) Our community can only improve on this situation by using collections of bursts which all have identical definitions for the Epeak calculation.
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Shivvers 2011 从射电余辉独立得到余辉喷流的总动能

主要内容:
1e52erg左右。方法是用Sedov-Taylor解+同步辐射

这里有将ST方法用到伽马暴里来的一个范例。

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文章信息:

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Title:
A Beaming-Independent Estimate of the Energy Distribution of Long Gamma-Ray Bursts: Initial Results and Future Prospects
Authors:
Shivvers, Isaac; Berger, Edo
Publication:
eprint arXiv:1101.0603
Publication Date:
01/2011
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
Submitted to ApJ; 11 pages, 5 figures, 2 tables
Bibliographic Code:
2011arXiv1101.0603S

Abstract

We present single-epoch radio afterglow observations of 24 long-duration gamma-ray burst (GRB) on a timescale of >100 d after the burst. These observations trace the afterglow evolution when the blastwave has decelerated to mildly- or non-relativistic velocities and has roughly isotropized. We infer beaming-independent kinetic energies using the Sedov-Taylor self-similar solution, and find a median value for the sample of detected bursts of about 7x10^51 erg, with a 90% confidence range of 1.1x10^50-3.3x10^53 erg. Both the median and 90% confidence range are somewhat larger than the results of multi-wavelength, multi-epoch afterglow modeling (including large beaming corrections), and the distribution of beaming-corrected gamma-ray energies. This is due to bursts in our sample with only a single-frequency observation for which we can only determine an upper bound on the peak of the synchrotron spectrum. This limitation leads to a wider range of allowed energies than for bursts with a well-measured spectral peak. Our study indicates that single-epoch centimeter-band observations covering the spectral peak on a timescale of ~1 yr can provide a robust estimate of the total kinetic energy distribution with a small investment of telescope time. The substantial increase in bandwidth of the EVLA (up to 8 GHz simultaneously with full coverage at 1-40 GHz) will provide the opportunity to estimate the kinetic energy distribution of GRBs with only a few hours of data per burst.
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星期五, 四月 01, 2011

Hakkila 2011 伽马暴脉冲的性质没有长短暴之分

主要内容:
不是说长的偏软短的偏硬不存在了,而是变化趋势是连续的。


精彩摘抄:

时间越长,辐射的能量越多

时间越长,谱越软

时间越长,峰值流量越小,反相关

时间越长,lag时间越长(我记得好像是反过来的呀,短暴的时延不是更明显的嘛)


文章信息:

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Title:
The Progenitor-Independent Nature of Gamma-Ray Burst Pulses
Authors:
Hakkila, JonPreece, Robert D.
Publication:
eprint arXiv:1103.5434
Publication Date:
03/2011
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
27 pages including 9 figures and 3 tables, submitted to The Astrophysical Journal
Bibliographic Code:
2011arXiv1103.5434H

Abstract

We demonstrate that a single, continuous set of correlated properties (duration, peak luminosity, time-integrated luminosity, spectral hardness, lag, and asymmetry) is present in all distinguishable gamma-ray burst pulses, regardless of whether these pulses originate in Long, Short, or Intermediate bursts. These properties correlate even in the observer's frame, indicating that intrinsic correlations are more pronounced than secondary effects resulting from relativistic cosmology such as the inverse square law and time dilation. We show how all correlated pulse characteristics are the direct result of hard-to-soft pulse evolution, and we demonstrate that "intensity tracking" pulses not having these properties are not single pulses; they instead appear to be composed of two or more overlapping hard-to-soft pulses. In order to better understand pulse characteristics, we recognize that hard-to-soft evolution provides a more accurate definition of a pulse than its intensity variation. This realization, coupled with the observation that pulses begin near-simultaneously across a wide range of energies, leads us to conclude that the observed pulse emission represents the energy decay resulting from an initial injection, and that one simple and as yet unspecified physical mechanism is likely to be responsible for all gamma-ray burst pulses regardless of the environment in which they form and the progenitors that supply them with energy.
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