2013之重要事件

（仅包括我关心的）
1. GRB 130427A

2. GRB 130603B

3. FRB

4. AMS2公布初步数据了

5. IceCube的两个高能中微子

Hambaryan, V. V. 2012 公元775/4年的C14增加可能是一个短暴

主要内容:

郁闷，我们想说它是伽马暴产生的，被人家先说了。

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Title:		A Galactic short gamma-ray burst as cause for the 14C peak in AD 774/5
Authors:		Hambaryan, V. V.; Neuhaeuser, R.
Publication:		eprint arXiv:1211.2584
Publication Date:		11/2012
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Comment:		MNRAS, accepted; 6 pages, 3 figures
Bibliographic Code:		2012arXiv1211.2584H

Abstract

In the last 3000 yr, one significant and rapid increase in the concentration of 14C in tree rings was observed; it corresponds to a gamma-ray energy input of 7x10^24 erg at Earth within up to one year in AD 774/5 (Miyake et al. 2012). A normal supernova and a solar or stellar flare are unlikely as cause (Miyake et al. 2012), so that the source remained unknown. Here, we show that a short gamma-ray burst (GRB) in our Galaxy is consistent with all observables: Such an event is sufficiently short and provides the necessary energy in the relevant spectral range of $\gamma$-rays. Its spectral hardness is consistent with the differential production rates of 14C and 10Be as observed. The absence of reports about a historic sighting of a supernova in AD 774/5 or a present-day supernova remnant are also consistent with a short GRB. We estimate the distance towards this short GRB to be ~ 1 to 4 kpc - sufficiently far away, so that no extinction event on Earth was triggered. This is the first evidence for a short GRB in our Galaxy.

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一些放在Dropbox上的参考资料

https://www.dropbox.com/sh/i50jq3ak47afxnf/Y9lhHkW2Yb?lst

包括天文常数，数学公式，物理公式，数学符号的latex写法，数学公式的英语读法等

Lei, Hai-Dong 2011 平降阶段的星风模型

主要内容:
星风环境下，减速时标以内时平降阶段，拐折是减速时标。

（这个也可以用来限制洛伦兹因子哦~ 就和光学的peak是一样的，不过要是发现有几个光学的peak和这个时标不一致就麻烦了，不过也可以说光学的是别的来源。）

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Title:		Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment
Authors:		Lei, Hai-Dong; Wang, Jiu-Zhou; Lü, Jing; Zou, Yuan-Chuan
Affiliation:		AA(), AB(), AC(), AD()
Publication:		Chinese Physics Letters, Volume 28, Issue 12, pp. 129801 (2011).
Publication Date:		12/2011
Origin:		IOP
DOI:		10.1088/0256-307X/28/12/129801
Bibliographic Code:		2011ChPhL..28l9801L

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.

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伽马暴光变的功率密度谱

有人做了GRB 080319B等的光变曲线的功率密度谱( http://grbcn.blogspot.com/2012/02/bhatt-nilay-2011.html )，虽然没看出什么周期性来，但应该也能看出什么东西吧。

如果把所有的暴都放在一起，是不是可以得到什么伽马暴的共性呢？

Nicuesa Guelbenzu, A. 2012 GRB090510的晚期余辉观测

主要内容:


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X射线和UVOT的观测。从拐折的时间上来看，很有可能第一个拐折是jet break，而第二个是频率穿过，穿过之后二者的时间指数就一样了，因为它们在同一个频率段。文章中并没有提到这个。

光学余辉



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Title:		The late-time afterglow of the extremely energetic short burst GRB 090510 revisited
Authors:		Nicuesa Guelbenzu, A.; Klose, S.; Kruehler, T.; Greiner, J.; Rossi, A.; Kann, D. A.; Olivares E., F.; Rau, A.; Afonso, P. M. J.;Elliott, J.; Filgas, R.; Kuepcue Yoldas, A.; McBreen, S.; Nardini, M.; Schady, P.; Schmidl, S.; Sudilovsky, V.; Updike, A. C.;Yoldas, A.
Publication:		eprint arXiv:1201.3885
Publication Date:		01/2012
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		submitted to Astronomy & Astrophysics, accepted for publication on Dec 24, 2011
Bibliographic Code:		2012arXiv1201.3885N

Abstract

The discovery of the short GRB 090510 has raised considerable attention mainly because it had a bright optical afterglow and it is among the most energetic events detected so far within the entire GRB population. The afterglow was observed with swift/UVOT and swift/XRT and evidence of a jet break around 1.5 ks after the burst has been reported in the literature, implying that after this break the optical and X-ray light curve should fade with the same decay slope. As noted by several authors, the post-break decay slope seen in the UVOT data is much shallower than the steep decay in the X-ray band, pointing to an excess of optical flux at late times. We reduced and analyzed new afterglow light-curve data obtained with the multichannel imager GROND. Based on the densely sampled data set obtained with GROND, we find that the optical afterglow of GRB 090510 did indeed enter a steep decay phase starting around 22 ks after the burst. During this time the GROND optical light curve is achromatic, and its slope is identical to the slope of the X-ray data. In combination with the UVOT data this implies that a second break must have occurred in the optical light curve around 22 ks post burst, which, however, has no obvious counterpart in the X-ray band, contradicting the interpretation that this could be another jet break. The GROND data provide the missing piece of evidence that the optical afterglow of GRB 090510 did follow a post-jet break evolution at late times.

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伽马暴作为高能辐射的来源

记得Tsvi他们曾经做过超新星作为超高能辐射的来源的，它们只能来自于银河系，或者较近的其它星系。但是为什么不能是伽马暴呢？

不过很可能不行，不然他们更自然地应该认为是伽马暴而不是超新星。（可能是爆发率的问题，银河系一百万年才有一次伽马暴，而超新星的频率更高。）

Castro Cerón 2010 伽马暴宿主星系的质量和SFR

主要内容:
说宿主星系都是低质量的star forming system，比field galaxy的平均质量都小。SFR，甚至specific star formation rate都比别人低。

为什么呢？
我觉得其它高SFR的星系应该有更多的伽马暴。原因会不会是高SSFR的星系的尘埃比较多，伽马射线出不来呢？

"the dust-uncorrected UV SFR"和做了修正的区别大吗？这里的SFR的范围是10^-2 M _sun yr^-1 < SFR < 10 M _sun yr^-1. 但是看另一篇文章，却是（0.03，300）！见ADS 2011ApJ...735L...8K， 或者：2010AJ....140.1557L

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Title:		On the Distribution of Stellar Masses in Gamma-ray Burst Host Galaxies
Authors:		Castro Cerón, J. M.; Michałowski, M. J.; Hjorth, J.; Malesani, D.; Gorosabel, J.; Watson, D.;Fynbo, J. P. U.; Morales Calderón, M.
Affiliation:		AA(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark;...)
Publication:		The Astrophysical Journal, Volume 721, Issue 2, pp. 1919-1927 (2010). (ApJ Homepage)
Publication Date:		10/2010
Origin:		IOP
ApJ Keywords:		cosmology: observations, dust, extinction, galaxies: fundamental parameters, galaxies: ISM, gamma-ray burst: general, infrared: galaxies
DOI:		10.1088/0004-637X/721/2/1919
Bibliographic Code:		2010ApJ...721.1919C

Abstract

We analyze Spitzer images of 30 long-duration gamma-ray burst (GRB) host galaxies. We estimate their total stellar masses (M_sstarf) based on the rest-frame K-band luminosities (L_{K_{rest}}) and constrain their star formation rates (SFRs; not corrected for dust extinction) based on the rest-frame UV continua. Further, we compute a mean M_⋆ /L_{K_{rest}} = 0.45 M_sun/L _sun. We find that the hosts are low M _sstarf, star-forming systems. The median M _sstarf in our sample (langM _sstarfrang = 10^9.7 M _sun) is lower than that of "field" galaxies (e.g., Gemini Deep Deep Survey). The range spanned by M _sstarf is 10⁷ M_sun < M _sstarf < 10¹¹ M _sun, while the range spanned by the dust-uncorrected UV SFR is 10^-2 M _sun yr^-1 < SFR < 10 M _sun yr^-1. There is no evidence for intrinsic evolution in the distribution of M _sstarf with redshift. We show that extinction by dust must be present in at least 25% of the GRB hosts in our sample and suggest that this is a way to reconcile our finding of a relatively lower UV-based, specific SFR (phi ≡ SFR/M _sstarf) with previous claims that GRBs have some of the highest phi values. We also examine the effect that the inability to resolve the star-forming regions in the hosts has on phi.This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.

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快速观测早期光学余辉的办法

利用前兆。

也就是说在伽马暴本身还没有触发的时候，就触发定位以及地面的fellow up观测。虽然会有一些以为是前兆，后面并没有跟着暴。但是总有一些是暴的，这样就观测到了暴同时的光学辐射。

不过如果前兆就是暴本身的一部分的话，那也仅仅是提早了观测时间，相当于观测到了一个更长的暴的光学余辉。

Czerny 2010 BATSE的极短暴

主要内容:
短于0.1秒的暴。但是从空间分布等来看，可能也就是一般的短暴。

也许可以分析一下它们的spectral time lag，因为他们时标比较短，比较容易分辨。

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Title:		Observational constraints on the nature of very short gamma-ray bursts
Authors:		Czerny, Bo\. zena; Janiuk, Agnieszka; Cline, David B.; Otwinowski, Stan
Publication:		eprint arXiv:1006.1470
Publication Date:		06/2010
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		25 pages, 14 figures; accepted to New Astronomy
Bibliographic Code:		2010arXiv1006.1470C

Abstract

We discuss a very peculiar subgroup of gamma-ray bursts among the BATSE sources. These bursts are very short ($T_{90} \le $0.1 s), hard, and came predominantly from a restricted direction of the sky (close to the Galactic anti-center). We analyze their arrival times and possible correlations, as well as the profiles of individual bursts. We find no peculiarities in the arrival times of Very Short Bursts (VSBs) despite their highly non-uniform spatial distribution. There is no dependence in the burst shapes on location. Bursts coming both from the burst-enhancement Galactic Anticenter region and from all other directions show considerable dispersion in their rise and fall times. Significant fraction of VSBs have multiple peaks despite their extremely short duration. Burst time properties are most likely to be consistent with two origin mechanisms: either with binary NS-NS mergers with low total masses passing through a phase of hypermassive neutron star, or with evaporation of the primordial black holes in the scenario of no photosphere formation.

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2009.9.14-9.18 威尼斯shocking universe会议

会议网址: http://www.brera.inaf.it/sanservolo2009/index.html

他们说要提供ppt的, 不知道为什么也没上网.

以下是会议日程. 大致第一天Swift相关；第二天Fermi相关；第三天半天, 比较杂；第四天比较关注宇宙方面的如宿主星系, 高红移；第五天的也比较杂.

(时间表拷贝自网站上)

Sunday - September 13th
18:00 - 20:00	Registration & Welcome Cocktail
Monday - September 14th
07:45 - 08:45	Registration
	Chairman	M. Feroci
08:45 - 09:00	G. Chincarini	Welcome 此人很像偷天陷阱里的男主角老头. 附剧照 http://posters.imdb.cn/jz/46852
09:00 - 09:35	M. Lyutikov	GRB: observational progress and theoretical problems 主要内容大致有(这里以及以下都包含严重的偏见和记忆误差): 1. 一共有8个想080513这样的, 可能是短暴加一个tail; 2. 暴本身阶段的低频端的硬谱可能来自电子的分布; 3.说080916C的同步辐射模型是不行的
09:35 - 09:50	I. Steele	Optical polarization measurements of GRB060418 and GRB090102 他们利物浦的望远镜加了偏振片, 这是两个观测. 其中060418的小于8%, 最令人惊讶的是090102的有10%, 而且致信度还很高!
09:50 - 10:05	C. Guidorzi	The controversial link between prompt optical and gammarays: temporal study of GRB 080319B 说这个暴的光变里有3.3s的周期现象. 下图是time lag
10:05 - 10:30	Coffee Break
10:30 - 10:55	S. Barthelmy	GRB Prompt Emission and Swift-BAT 图左显示了三个仪器的分布和E_p的分布 1. 统计上, pulse的宽度 W~E_p^-0.4~z^0.4 2. 谱形上, cutoff power law的比Band的还多 3. 观测上, Swift的高红移的暴并没有更软 (这个可能说明E_p比较大, 即使红移比较高, 还是没看到peak的地方； 或者谱整个是一个比较好的幂律, 这样也不会看到变软； 或者, 当然最直接的解释应该是高红移的暴本身比较硬.) 4. 他们Swift在准备 sub-threshold, 就是不要那么强的伽玛光子信号就触发. 这样可以看到更多弱暴, 虽然会有很多误触发.
10:55 - 11:20	S. Kobayashi	Magnetized Fireballs and Early Afterglows
11:20 - 11:45	A. Pe'er	Observations, theory and implications of thermal emission from gamma-ray bursts 他主要还是说他的Themal component
11:45 - 12:05	L. Amati	Spectrum-energy correlation in GRB: status and perspectives 会议上有两个报告说Amati关系不对, 让他很郁闷. 在Tsvi的报告提问阶段都快结束后强烈要求发言, 终于给他机会, 说了很大一通. 最后说你们不能这样, 搞的让大家以为我这个关系真的就是错的样. Tsvi听了半天, 然后回了一句话, 闪人. 没听大明白, 大意是它是错的就是错的.
12:05 - 12:30	J. Racusin	Jet Breaks and Energetics of Swift GRB X-ray Afterglows
12:30 - 12:45	D. Burrows	Chandra Searches for Jet Breaks 几类光变所占的比例.
12:45 - 13:00	P. Evans	Confronting GRB afterglow models with a complete set of XRT light curves and hardness ratios
13.00 - 14.20	Lunch
	Chairman	S. Barthelmy
14:20 - 14:45	A. MacFadyen	GRB Afterglow Lightcurves from Multi-Dimensional Simulations
14:45 - 15:10	R. Margutti	GRB temporal structure: flares and short term variability
15:10 - 15:30	R. Yamazaki	Prior Emission Model for the Plateau Phase in the X-ray Afterglow
15:30 - 15:55	E. Del Monte	The observation of Gamma Ray Bursts with AGILE
15:55 - 16:10	R. Klebesadel	The Discovery of Cosmic Gamma-Ray Bursts 此人算是伽玛暴的开山鼻祖, 1973?年发表了第一篇观测到伽玛暴的文章. 不知道会议组怎么这么有能耐, 居然能请到他来. 讲完后以及提问完后迎来了会上最长时间的掌声, 起码有一分钟. 具体内容不是很有意思, 提问还是蛮有意思的. Kouveliotou问他为什么那么晚才发文章, 他解释说忙, 还有因为计算机故障还是什么. 据说还有另外的版本, 说是因为军事机密问题, 不能发. (参见伽玛暴的发现的相关内容) 由于Vela是军事卫星, 主要目的是看前苏联有没有搞秘密核试验. 所以有人就问那你们到底看到了没有, 他坚决不泄密.
16:10 - 16:35	Coffee Break
16:35 - 17:00	F. Daigne	The prompt emission of gamma-ray bursts in the internal shock model
17:00 - 17:15	S. Sugita	Timing and spectral analysis of Short GRB and Multi-spiked Long GRB
17:15 - 17:30	E. Liang	Single Power-Law Decaying XRT lightcurves and Implications for the Unified Origin of the X-rays
17:30 - 17:45	P. Roming	A Large Homogenous Sample of Optical GRB Afterglow Light Curves
17:45 - 18:00	M. De Pasquale	Chromatic evolution in GRB afterglows
18:00 - 18:20	S. Covino	Optical observations of GRB afterglows
18:20 - 18:35	J. Nousek	Status of the Swift Mission
Tuesday - September 15th
	Chairman	P. Michelson
09:00 - 09:25	N. Omodei	Gamma-Ray Burst at HighEnergy: the Fermi LAT first observation of the shocking Universe
09:25 - 09:45	N. Kawai	Pulse structures of GRB 080916C observed with Fermi LAT/GBM
09:45 - 10:05	S. Guiriec	GRB 090510, a short and hard burst detected by Fermi
10:05 - 10:25	F. De Palma	GRB 090902B, a long GRB with High Energy emission detected with Fermi
10:25 - 11:00	Coffee Break
11:00 - 11:20	E. Bissaldi	GRB 090323 and GRB 090328: two ksec long high-energy GammaRay Bursts detected with Fermi
11:20 - 11:45	B. Paciesas	Fermi GBM results
11:45 - 12:10	M. Briggs	Spectral Evolution of Three Short GRBs on Fine Timescales
12:10 - 12:30	V. Connaughton	High-Energy Spectral signatures of LAT-detected short gamma-ray bursts
12:30 - 12:55	J. Granot	Some Implications of Fermi High-Energy GRB Observations
12.55 - 14.20	Lunch
	Chairman	R. Bellazzini
14:20 - 14:45	K. Asano	Theoretical Interpretation for Fermi LAT-detected Gamma-ray Bursts
14:45 - 15:10	C. Dermer	Evidence for Ultra-High Energy Cosmic Ray Acceleration from Fermi Observations of GRBs
15:10 - 15:35	P. Michelson	Fermi LAT results
15:35 - 16:00	B. Atwood	Fermi-LAT Analysis to Maximize GRB Science
16:00 - 16:30	Coffee Break
16:30 - 16:50	D. Kocevski	LAT Upper Limits to GRBs
16:50 - 17:05	T. Aune	Constraints on GeV-TeV Emission from the "nakedeye" GRB 080319B
17:05 - 17:30	Y. Fan	Interpretation and implication of the non-detection of GeV spectrum excess by Fermi gamma-ray Space Telescope in most GRBs
17:30 - 17:45	A. Melandri	The Rise and Fall of GRBs - Lorentz Factors and Fireball Shock Physics
17:45 - 18:10	R. Barniol-Duran	High energy photons from Fermi GRBs: Who would have thought that they were produced in the external shock?
19:15	Visit at the S. Marco Basilica
Wednesday - September 16th
	Chairman	P. Roming
09:00 - 09:30	E. Berger	The Host Galaxies of Short GRBs: Implications for the Progenitors and Comparison to Long GRB Hosts
09:30 - 09:45	F. Virgili	Are all short GRBs of compact star merger origin?
09:45 - 10:00	P. D'Avanzo	Optical spectroscopy of short GRB afterglows
10:00 - 10:20	W. Lee	The role of winds and tidal tails from post merger disks in the production of outflows and late time flares in SGRBs
10:20 - 10:40	Poster competition
10:40 - 11:10	Coffee Break
11:10 - 11:40	C. Fryer	Neutrinos and Gravitational Waves from Long Duration GRBs
11:40 - 12:05	P. Vreeswijk	GRB optical afterglow spectroscopy and host galaxies: an unbiased approach
12:05 - 12:20	D. Perley	The Environments of Dark Gamma-Ray Bursts
12:20 - 12:35	A. De Ugarte Postigo	GRB 090313: X-shooter's first glimpse of a GRB
12:35 - 13:15	K. Hamaguchi	News on Eta-Carinae
13:15	Lunch
13:45	Free Afternoon - Social Trip to S. Francesco del Deserto island
Thursday - September 17th
	Chairman	J. Osborne
09:00 - 09:25	S. Savaglio	Gamma-Ray Burst Host Galaxies and the High Redshift Universe
09:25 - 09:50	A. Fruchter	Environments, Hosts, and their Implications for the Physics and Progenitors of GRBs
09:50 - 10:05	E. Levesque	Modeling the Host Galaxies of Long-Duration Gamma-Ray Bursts
10:05 - 10:20	P. Schady	Dust Extinction Properties within GRB Host Galaxies
10:20 - 10:35	K. Svensson	The host galaxies of core-collapse supernovae and gamma ray bursts
10:35 - 11:00	Coffee Break
11:00 - 11:30	A. Soderberg	A Holistic View of the GRB-SN Connection
11:30 - 11:55	M. Della Valle	GRB-SN Connection: observational outcomes
11:55 - 12:15	S. Nagataki	GRB-SN Connection: Central Engine of Long GRBs and Explosive Nucleosynthesis
12:15 - 12:30	A. Kamble	XRF080109/SN2008D : an investigation at radio frequencies
12:30 - 12:45	R. Shen	The late jet in GRBs and its interactions with a supernova ejecta and a cocoon
12:45 - 13:00	F. De Colle	Bipolar Supernova Explosions: Nucleosynthesis and the Role of Magnetic Fields
13.00 - 14.30	Lunch
	Chairman	N. Kawai
14:30 - 15:00	P. Kumar	The Physics of GRB Prompt Emission
15:00 - 15:30	B. Zhang	GRB prompt emission models: from low sigma to high sigma
15:30 - 16:00	T. Piran	TBA
16:00 - 16:30	Coffee Break
16:30 - 16:45	E. Nakar	Introduction for a debate
16:45 - 17:20		Debate: where do we stand?
17:20 - 17:35	A. Levan	Illuminating the dark ages with GRB 090423
17:35 - 17:50	R. Salvaterra	GRB 090423 reveals an exploding star at the epoch of reionization
17:50 - 18:05	D. Frail	Discovery of the Radio Afterglow from GRB 090423
18:05 - 18:20	A. Cucchiara	GRB 090429B as the second "extreme redshift" gamma-ray burst
18:20 - 18:45	T. Totani	GRBs and High Redshift Universe: High Redshift Galaxies, Pop III Stars, and Reionization
20:30	Social Dinner
Friday - September 18th
	Chairman	K. Hurley
08:45 - 09:10	C. Kouveliotou	Magnetar Observations with Fermi/GBM
09:10 - 09:25	S. Dall'Osso	Magnetars at birth as strong sources of Gravitation Wave Radiation
09:25 - 09:40	Y. Nakagawa	Suzaku Observations of Short Bursts from SGR 0501+4516
09:40 - 10:10	E. Ramirez-Ruiz	Compact Objects in The Era of Celestial Cinematography
10:10 - 10:40	Coffee Break
10:40 - 11:05	V. D'Elia	UVES-VLT High Resolution Spectroscopy of Gamma-Ray Burst afterglows: host galaxies and intervening absorbers
11:05 - 11:20	S. Vergani	Statistics and characteristics of MgII absorbers along GRB lines of sight observed with VLT-UVES
11:20 - 11:35	S. Campana	Circumburst ambient surrounding GRBs in the X-ray band
11:35 - 11:50	C. Thoene	GRB 090426 - a new class or a strange environment?
11:50 - 12:00	I. Horvath	GRB groups observed by BATSE, BeppoSAX and Swift
12:00 - 12:15	D. Lopez-Camara	Quiescence and late time activity in collapsars due to critical angular momentum distributions
12:15 - 12:30	G. Beskin	Discovery of the "central engine" manifestation in the Naked-Eye Burst prompt optical emission
12.30 - 14.00	Lunch
	Chairman	D. Burrows
14:00 - 14:25	K. Yamaoka	Suzaku observations of GRB prompt emissions and X-ray afterglows
14:25 - 14:55	C. Bianco	The extended afterglow luminosity evolution over the equitemporal surfaces
14:55 - 15:10	F. Genet	Steep decay phase and prompt emission models
15:10 - 15:25	V. Mangano	Modeling the spectral evolution in the decaying tails of Swift GRBs
15:25 - 15:45	S. Inoue	Probing UV radiation fields and magnetic fields in the era of first star formation through GeV γ-rays from very high-z GRBs
15:45 - 16:00	P. Romano	Supergiant Fast X-ray Transients: the Swift monitoring program
16:00 - 16:45	N. Gehrels	Concluding Remarks