Birnbaum 2011 检查时间零点移动后的外激波光学辐射

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应该不能被观测到，发现基本还是可以和观测不矛盾的。

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Title:		Observational constraints on the external shock prior emission hypothesis of GRBs
Authors:		Birnbaum, Tesla; Zhang, Bing; Zhang, Bin-Bin; Liang, En-Wei
Publication:		eprint arXiv:1105.5126
Publication Date:		05/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Bibliographic Code:		2011arXiv1105.5126B

Abstract

An intriguing hypothesis, i.e. there exists a decaying X-ray emission component before the GRB trigger, has been suggested to interpret the shallow decay phase of the X-ray afterglow detected in many {\em Swift} GRBs. If this "prior emission" is from an external shock, one would expect a corresponding optical emission component during the GRB prompt emission phase. In this paper we apply the available prompt optical emission data (both detections and upper limits) to constrain such a scenario. We fit the shallow and normal decay segments of the XRT light curves with a $T_0$-shifted single power law, and extrapolate the X-ray flux back to the time of the early optical observations. We then use the synchrotron spectrum predicted by the standard external shock model to extrapolate from the X-ray flux to the optical band, and obtain the possible range of the predicted optical flux. Finally, we compare the predictions with the observations. In the cases where later optical data are available, we also compare the shapes of the optical light curves to the predicted optical light curves from the external shock prior emission model. Overall, we find that the available optical data still allow the existence of an external shock prior emission component, although contrived parameters are required for some GRBs. In several cases, the detected optical emission must not be dominated by the prior emission component, and is likely associated with the second explosion that gives rise to the GRB itself.

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Cucchiara 2011 发现了红移为9.4的暴 090429B

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红线是定红移的地方

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Title:		A Photometric Redshift of z ~ 9.4 for GRB 090429B
Authors:		Cucchiara, A.; Levan, A. J.; Fox, D. B.; Tanvir, N. R.; Ukwatta, T. N.; Berger, E.; Krühler, T.;Küpcü Yoldaş, A.; Wu, X. F.; Toma, K.; Greiner, J.; Olivares E., F.; Rowlinson, A.; Amati, L.; Sakamoto, T.;Roth, K.; Stephens, A.; Fynbo, J. P. U.; Hjorth, J.; Malesani, D.; Jakobsson, P.; Wiersema, K.; O'Brien, P. T.;Soderberg, A. M.; Foley, R. J.; Fruchter, A. S.; Rhoads, J.; Rutledge, R. E.; Schmidt, B. P.; Dopita, M. A.;Podsiadlowski, P.; Willingale, R.; Wolf, C.; Kulkarni, S. R.; D'Avanzo, P.
Publication:		eprint arXiv:1105.4915
Publication Date:		05/2011
Origin:		ARXIV
Keywords:		Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		Accepted for publication on The Astrophysical Journal
Bibliographic Code:		2011arXiv1105.4915C

Abstract

Gamma-ray bursts (GRBs) serve as powerful probes of the early Universe, with their luminous afterglows revealing the locations and physical properties of star forming galaxies at the highest redshifts, and potentially locating first generation (Population III) stars. Since GRB afterglows have intrinsically very simple spectra, they allow robust redshifts from low signal to noise spectroscopy, or photometry. Here we present a photometric redshift of z~9.4 for the Swift-detected GRB 090429B based on deep observations with Gemini-North, the Very Large Telescope, and the GRB Optical and Near-infrared Detector. Assuming a Small Magellanic Cloud dust law (which has been found in a majority of GRB sight-lines), the 90% likelihood range for the redshift is 9.06 < z < 9.52, although there is a low-probability tail to somewhat lower redshifts. Adopting Milky Way or Large Magellanic Cloud dust laws leads to very similar conclusions, while a Maiolino law does allow somewhat lower redshift solutions, but in all cases the most likely redshift is found to be z>7. The non-detection of the host galaxy to deep limits (Y_AB >~ 28 mag, which would correspond roughly to 0.001 L* at z=1) in our late time optical and infrared observations with the Hubble Space Telescope strongly supports the extreme redshift origin of GRB 090429B, since we would expect to have detected any low-z galaxy, even if it were highly dusty. Finally, the energetics of GRB 090429B are comparable to those of other GRBs, and suggest that its progenitor is not greatly different to those of lower redshift bursts.

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Woosley 2011 伽马暴前身星综述

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也提到中心引擎，还有超长的低能暴（没观测到）。

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Title:		Models for Gamma-Ray Burst Progenitors and Central Engines
Authors:		Woosley, S. E.
Publication:		eprint arXiv:1105.4193
Publication Date:		05/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		31 pages, 1 figure, to be published by Cambridge University Press in the volume "Gamma-Ray Bursts". Final version accepted for publication June 23, 2010
Bibliographic Code:		2011arXiv1105.4193W

Abstract

Most gamma-ray bursts are made during the deaths of massive stars. Here the environmental circumstances, stellar evolutionary paths, and explosion physics that might produce the bursts are reviewed. Neither of the two leading models - collapsar and millisecond magnetar - can be excluded, and both may operate in progenitor stars of different masses, metallicities, and rotation rates. Potential diagnostics are discussed and uncertainties highlighted. Both models are capable of producing a wide variety of transients whose properties vary with both stellar properties and viewing angle. Some of these are reviewed including the possibility of very long (days) low luminosity bursts, so far undiscovered, short hard bursts from massive stellar progenitors, and bursts from very massive Population III stars.

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Thöne 2011 GRB 101225A可能是类似于XRF 060218的shock breakout

主要内容:
红移=0.32是估计出来的，方法是说外流的速度应该在0.03c到0.5c之间，加上是黑体辐射，估算了红移的范围。（不知道为什么就估算出来了，貌似文章也没说，就一句话）
然后把060218的光变移到0.32的时候和观测到的101225a的很像，就说这个圣诞暴的红移是0.32 =_=!


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Title:		An unusual stellar death on Christmas Day
Authors:		Thöne, C. C.; de Ugarte Postigo, A.; Fryer, C. L.; Page, K. L.; Gorosabel, J.; Perley, D. A.; Kouveliotou, C.; Janka, H. T.; Aloy, M. A.; Mimica, P.; Racusin, J. L.; Krimm, H.; Cummings, J.; Oates, S. R.; Holland, S. T.; Siegel, M. H.; De Pasquale, M.; Sonbas, E.; Im, M.; Park, W. -K.; Kann, D. A.; Guziy, S.; Hernandez Garcia, L.; Bundy, K.; Castro-Tirado, A. J.; Choi, C.; Jeong, H.; Korhonen, H.; Kubanek, P.; Lim, J.; Llorente, A.; Moskvitin, A.; Muñoz Darias, T.; Pak, S.; Parrish, I.
Publication:		eprint arXiv:1105.3015
Publication Date:		05/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		19 pages, 20 figures, submitted
Bibliographic Code:		2011arXiv1105.3015T

Abstract

Massive stars can end their lives in many different ways. Long Gamma-Ray Bursts (GRBs) are the most dramatic examples, releasing ultra-relativistic ejecta that produce non-thermal emission when interacting with the surrounding medium (Zhang et al. 2004). Usually, those events are accompanied by a supernova (SN) (Woosley et al. 2006). In a few low-redshift GRB-SNe we could observe the actual breakout of the shock front from the surface of the star (Campana et al. 2006). Here we present GRB 101225A, a very peculiar event at a distance of 1.6 Gpc. A bright X-ray transient with a thermal component and an unusual optical counterpart followed an exceptionally long gamma-ray event. During the first 10 days, the optical emission evolved as an expanding, cooling blackbody with a large initial radius, after which a faint SN was observed. The absence of a normal GRB afterglow implies that some dense material, likely ejected by the progenitor star, completely thermalized the high-energy emission. A possible progenitor is a helium star/neutron star binary which underwent a common envelope phase, expelling its hydrogen envelope prior to the explosion. The final merging process created a GRB-like event where we observe the shock breakout of the secondary star before the high-energy emission gets thermalized in the collision with the previously expelled shell, until finally the emission from the SN itself takes over. GRB 101225A defines a new, rare type of blackbody-dominated GRB which explodes in a dense environment created by the progenitor system itself.

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Quataert 2011 GRB 110328A的超长暴模型

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Title:		Swift 1644+57: The Longest Gamma-ray Burst?
Authors:		Quataert, Eliot; Kasen, Dan
Publication:		eprint arXiv:1105.3209
Publication Date:		05/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		submitted to MNRAS Letters
Bibliographic Code:		2011arXiv1105.3209Q

Abstract

Swift recently discovered an unusual gamma-ray and x-ray transient (Sw 1644+57) that was initially identified as a long-duration gamma-ray burst (GRB). However, the ~ 10 keV x-ray emission has persisted for over a month with a luminosity comparable to its peak value. The astrometric coincidence of the source with the center of its host galaxy, together with other considerations, motivated the interpretation that Sw 1644+57 was produced by an outburst from a 10^{6-7} M_sun black hole at the center of the galaxy. Here we consider the alternate possibility that Sw 1644+57 is indeed a long-duration GRB, albeit a particularly long one. We discuss the general properties of very long-duration, low-power GRB-like transients associated with the core-collapse of a massive star. Both neutron star (magnetar) spindown and black hole accretion can power such events. The requirements for producing low-power, very long-duration GRBs by magnetar spindown are similar to those for powering extremely luminous supernovae by magnetar spindown, suggesting a possible connection between these two unusual types of transients. Alternatively, Sw 1644+57 be associated with the faintest core-collapse explosions: the collapse of a rotating red supergiant in a nominally failed supernova can power accretion onto a solar-mass black hole for up to ~ 100 days; the jet produced by black hole accretion inevitably unbinds the outer envelope of the progenitor, leading to a weak ~ 10^{49} erg explosion. In both neutron star and black hole models, a jet can burrow through the host star in a few days, with a kinetic luminosity ~ 10^{45-46} ergs/s, sufficient to power the observed emission of Sw 1644+57.

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Shao 2011 GRB 110328A的超长暴模型

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Title:		Sw 1644+57/GRB 110328A: the physical origin and the composition of the relativistic outflow
Authors:		Shao, Lang; Zhang, Fu-Wen; Fan, Yi-Zhong; Wei, Da-Ming
Publication:		eprint arXiv:1104.4685
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		10 pages, 1 figure
Bibliographic Code:		2011arXiv1104.4685S

Abstract

Sw 1644+57/GRB 110328A is a remarkable cosmological X-ray outburst detected by the {\it Swift} satellite. Its early-time ($t\lesssim 0.1$ day since the trigger) X-ray emission resembles some Gamma-Ray Bursts (GRBs), say, GRB 090417B. But the late-time flaring X-ray plateau lasting $> 20$ days renders it unique. We examine the possibilities that the outburst is a super-long GRB powered either by the fallback accretion onto a nascent black hole or by a millisecond pulsar, and find out that these two scenarios can address some but not all of the main observational features. We then focus on the model of tidal disruption of a (giant) star by a massive black hole. The mass of the tidal-disrupted star is estimated to be $\gtrsim$ a few solar masses. A simple/straightforward argument for a magnetic origin of the relativistic outflow has been presented.

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Sakamoto 2011 Swift BAT catalog 2

主要内容:
从2004年到2009年476个暴的数据。

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Title:		The Second Swift BAT Gamma-Ray Burst Catalog
Authors:		Sakamoto, T.; Barthelmy, S. D.; Baumgartner, W. H.; Cummings, J. R.; Fenimore, E. E.; Gehrels, N.; Krimm, H. A.; Markwardt, C. B.; Palmer, D. M.; Parsons, A. M.; Sato, G.; Stamatikos, M.; Tueller, J.; Ukwatta, T. N.; Zhang, B.
Publication:		eprint arXiv:1104.4689
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		65 pages, 33 figures, 13 tables, Accepted in ApJS, Nine machine-readable tables are available at http://swift.gsfc.nasa.gov/docs/swift/results/bat2_catalog/
Bibliographic Code:		2011arXiv1104.4689S

Abstract

We present the second Swift Burst Alert Telescope (BAT) catalog of gamma-ray bursts (GRBs), which contains 476 bursts detected by the BAT between 2004 December 19 and 2009 December 21. This catalog (hereafter the BAT2 catalog) presents burst trigger time, location, 90% error radius, duration, fluence, peak flux, time-averaged spectral parameters and time-resolved spectral parameters measured by the BAT. In the correlation study of various observed parameters extracted from the BAT prompt emission data, we distinguish among long-duration GRBs (L-GRBs), short-duration GRBs (S-GRBs), and short-duration GRBs with extended emission (S-GRBs with E.E.) to investigate differences in the prompt emission properties. The fraction of L-GRBs, S-GRBs and S-GRBs with E.E. in the catalog are 89%, 8% and 2% respectively. We compare the BAT prompt emission properties with the BATSE, BeppoSAX and HETE-2 GRB samples. We also correlate the observed prompt emission properties with the redshifts for the GRBs with known redshift. The BAT T90 and T50 durations peak at 70 s and 30 s, respectively. We confirm that the spectra of the BAT S-GRBs are generally harder than those of the L-GRBs. The time-averaged spectra of the BAT S-GRBs with E.E. are similar to those of the L-GRBs. Whereas, the spectra of the initial short spikes of the S-GRBs with E.E. are similar to those of the S-GRBs. We show that the BAT GRB samples are significantly softer than the BATSE bright GRBs, and that the time-averaged Epeak of the BAT GRBs peaks at 80 keV which is significantly lower energy than those of the BATSE sample which peak at 320 keV. The time-averaged spectral properties of the BAT GRB sample are similar to those of the HETE-2 GRB samples. By time-resolved spectral analysis, we find that only 10% of the BAT observed photon indices are outside the allowed region of the synchrotron shock model.

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Gruber 2011 GBM观测到的32个暴

主要内容:
由于GBM和BATSE差不多，观测到的暴的性质也差不多，峰值能量在800keV，不想Swift的BAT。

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Title:		Rest-frame properties of 32 gamma-ray bursts observed by the Fermi Gamma-Ray Burst Monitor
Authors:		Gruber, D.; Greiner, J.; von Kienlin, A.; Rau, A.; Briggs, M. S.; Connaughton, V.; Goldstein, A.; van der Horst, A. J.; Nardini, M.; Bhat, P. N.; Bissaldi, E.; Burgess, J. M.; Chaplin, V. L.; Diehl, R.; Fishman, G. J.; Fitzpatrick, G.; Foley, S.; Gibby, M. H.; Giles, M. M.; Guiriec, S.; Kippen, R. M.; Kouveliotou, C.; Lin, L.; McBreen, S.; Meegan, C. A.; Olivares E., F.; Paciesas, W. S.; Preece, R. D.; Tierney, D.; Wilson-Hodge, C.
Publication:		eprint arXiv:1104.5495
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		accepted by A&A
Bibliographic Code:		2011arXiv1104.5495G

Abstract

Aims: In this paper we study the main spectral and temporal properties of gamma-ray bursts (GRBs) observed by Fermi/GBM. We investigate these key properties of GRBs in the rest-frame of the progenitor and test for possible intra-parameter correlations to better understand the intrinsic nature of these events. Methods: Our sample comprises 32 GRBs with measured redshift that were observed by GBM until August 2010. 28 of them belong to the long-duration population and 4 events were classified as short/hard bursts. For all of these events we derive, where possible, the intrinsic peak energy in the $\nu F_{\nu}$ spectrum (\eprest), the duration in the rest-frame, defined as the time in which 90% of the burst fluence was observed (\tninetyrest) and the isotropic equivalent bolometric energy (\eiso). Results: The distribution of \eprest has mean and median values of 1.1 MeV and 750 keV, respectively. A log-normal fit to the sample of long bursts peaks at ~800 keV. No high-\ep population is found but the distribution is biased against low \ep values. We find the lowest possible \ep that GBM can recover to be ~ 15 keV. The \tninetyrest distribution of long GRBs peaks at ~10 s. The distribution of \eiso has mean and median values of $8.9\times 10^{52}$ erg and $8.2 \times 10^{52}$ erg, respectively. We confirm the tight correlation between \eprest and \eiso (Amati relation) and the one between \eprest and the 1-s peak luminosity ($L_p$) (Yonetoku relation). Additionally, we observe a parameter reconstruction effect, i.e. the low-energy power law index $\alpha$ gets softer when \ep is located at the lower end of the detector energy range. Moreover, we do not find any significant cosmic evolution of neither \eprest nor \tninetyrest.

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Shao 2011 某些短暴可能实际上是长暴

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主要从余辉的光变曲线上看。

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Title:		Implications for Understanding Short Gamma-Ray Bursts Detected by {\it Swift}
Authors:		Shao, Lang; Dai, Zi-Gao; Fan, Yi-Zhong; Zhang, Fu-Wen; Jin, Zhi-Ping; Wei, Da-Ming
Publication:		eprint arXiv:1104.5498
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:		10 pages, 5 figues, 2 tables
Bibliographic Code:		2011arXiv1104.5498S

Abstract

In an effort to understand the puzzle of classifying Gamma-Ray Bursts (GRBs), we have a systematic study of {\it Swift} GRBs and investigate several issues on short GRBs. Though short GRBs have a short ($\lesssim2$ s) prompt duration as monitored by {\it Swift} Burst Alert Telescope (BAT), the composite light curves including both the prompt and afterglow emission suggest that most of them have a similar radiative feature as the long GRBs. Besides, some well-studied short GRBs might also have an intrinsically long prompt duration, which renders them a type of short GRB imposters. Genuine short GRBs might be rare so that to discriminate the observed short GRBs is, not surprisingly, troublesome. In particular, the observational biases in the host identification and redshift measurement of GRBs should be taken with great caution. The redshift distribution which has been proposed to be different for long and short GRBs might have been strongly affected by the measurement methods.

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Nagakura 2011 数值模拟大质量恒星产生伽马暴

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二维，既有盘，也有包层，在一定条件下喷流可以冲出包层。

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Title:		Population III Gamma-Ray Bursts and Breakout Criteria for Accretion-Powered Jets
Authors:		Nagakura, Hiroki; Suwa, Yudai; Ioka, Kunihito
Publication:		eprint arXiv:1104.5691
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		37 pages, 16 figures, Submitted to ApJ
Bibliographic Code:		2011arXiv1104.5691N

Abstract

We investigate the propagations of accretion-powered jets in various types of massive stars such as Wolf-Rayet stars, light Population III (Pop III) stars, and massive Pop III stars, all of which are the progenitor candidates of Gamma-Ray Bursts (GRBs). We perform two dimensional axisymmetric simulations of relativistic hydrodynamics taking into account both the envelope collapse and the jet propagation (i.e., the negative feedback of the jet on the accretion). We calculate the accretion rate from the mass flux going through the inner boundary, and inject the jet with a constant accretion-to-jet conversion efficiency $\eta$. By varying the efficiency $\eta$ and opening angle $\theta_{op}$ for more than 30 models, we find that the forward shock wave succeeds to break out of the stellar surface and potentially create GRBs in all types of progenitors if a simple condition $\eta \gtrsim 10^{-3} (\theta_{op}/20^{\circ})^2$ is satisfied, that is consistent with analytical estimates, otherwise no explosion or some failed spherical explosions occur. We also suggest that a (slightly) delayed jet injection is preferred for GRBs.

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Mészáros 2011 磁化shell的碰撞产生GeV辐射

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从基本的动力学出发，考虑碰撞和辐射，值得读，看看具体怎么操作的--有些舍去、有些得考虑。

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Title:		GeV Emission from Collisional Magnetized Gamma Ray Bursts
Authors:		Mészáros, P.; Rees, M. J.
Publication:		eprint arXiv:1104.5025
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		ApJ(Lett.), in press
Bibliographic Code:		2011arXiv1104.5025M

Abstract

Magnetic fields may play a dominant role in gamma-ray bursts, and recent observations by the Fermi satellite indicate that GeV radiation, when detected, arrives delayed by seconds from the onset of the MeV component. Motivated by this, we discuss a magnetically dominated jet model where both magnetic dissipation and nuclear collisions are important. We show that, for parameters typical of the observed bursts, such a model involving a realistic jet structure can reproduce the general features of the MeV and a separate GeV radiation component, including the time delay between the two. The model also predicts a multi-GeV neutrino component.

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Cano 2011 对XRF 100316D / SN 2010bh的超新星部分的观测

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多个超新星/伽马暴的光学光变

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Title:		XRF 100316D / SN 2010bh and the Nature of Gamma Ray Burst Supernovae
Authors:		Cano, Z.; Bersier, D.; Guidorzi, C.; Kobayashi, S.; Levan, A. J.; Tanvir, N. R.; Wiersema, K.; D'Avanzo, P.; Fruchter, A. S.; Garnavich, P.; Gomboc, A.; Gorosabel, J.; Kasen, D.; Kopac, D.; Margutti, R.; Mazzali, P. A.; Melandri, A.; Mundell, C. G.; Nugent, P. E.; Pian, E.; Smith, R. J.; Steele, I.; Wijers, R. A. M. J.; Woosley, S. E.
Publication:		eprint arXiv:1104.5141
Publication Date:		04/2011
Origin:		ARXIV
Keywords:		Astrophysics - Solar and Stellar Astrophysics
Comment:		Sumitted to ApJ (27-April-2011). 17 pages, 11 figures and 8 tables
Bibliographic Code:		2011arXiv1104.5141C

Abstract

We present ground-based and HST optical and infrared observations of XRF 100316D / SN 2010bh. It is seen that the optical light curves of SN 2010bh evolve at a faster rate than the archetype GRB-SN 1998bw, but at a similar rate to SN 2006aj, a supernova that was spectroscopically linked with XRF 060218, and at a similar rate to non-GRB associated type Ic SN 1994I. We estimate the rest-frame extinction of this event from our optical data to be E(B-V)=0.18 +/- 0.08 mag. We find the V-band absolute magnitude of SN 2010bh to be M_{V}=-18.62 +/- 0.08, which is the faintest peak V-band magnitude observed to-date for a spectroscopically-confirmed GRB-SNe. When we investigate the origin of the flux at t-t_{o}=0.598 days, it is shown that the light is not synchrotron in origin, but is likely coming from the supernova shock break-out. We then use our optical and infrared data to create a quasi-bolometric light curve of SN 2010bh which we model with a simple analytical formula. The results of our modeling imply that SN 2010bh synthesized a nickel mass of M_{Ni}=0.10 +/- 0.01 M_{\odot}, ejected M_{ej}=2.24 +/- 0.08 M_{\odot} and has an explosion energy of E_{k}=1.39 +/- 0.06 x 10^{52} erg (where the quoted errors are statistical only; we discuss the potential sources of the systematic errors in the text). Finally, for a sample 20 GRB-SNe we check for a correlation between the stretch factors and luminosity factors in the R band and conclude that no statistically-significant correlation exists.

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