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.

显示标签为“5.3 time lag”的博文。显示所有博文
显示标签为“5.3 time lag”的博文。显示所有博文

星期二, 二月 07, 2012

Ukwatta, T. N. 2011 time lag--luminosity关系

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Title:
The lag-luminosity relation in the GRB source frame: an investigation with Swift BAT bursts
Authors:
Ukwatta, T. N.; Dhuga, K. S.; Stamatikos, M.; Dermer, C. D.; Sakamoto, T.; Sonbas, E.; Parke, W. C.; Maximon, L. C.;Linnemann, J. T.; Bhat, P. N.; Eskandarian, A.; Gehrels, N.; Abeysekara, A. U.; Tollefson, K.; Norris, J. P.
Affiliation:
AA(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AB(Department of Physics, The George Washington University, Washington, DC 20052, USA), AC(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; Center for Cosmology and Astro-Particle Physics (CCAPP) Fellow, Department of Physics, The Ohio State University, Columbus, OH 43210, USA), AD(Space Science Division, Code 7653, Naval Research Laboratory, Washington, DC 20375, USA), AE(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; Center for Research and Exploration in Space Science and Technology (CRESST), NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AF(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; Department of Physics, University of Adıyaman, 02040 Adıyaman, Turkey; Universities Space Research Association, 10211 Wincopin Circle, Suite 500, Columbia, MD 21044-3432, USA), AG(Department of Physics, The George Washington University, Washington, DC 20052, USA), AH(Department of Physics, The George Washington University, Washington, DC 20052, USA), AI(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA), AJ(University of Alabama in Huntsville Center for Space Plasma and Aeronomic Research, 320 Sparkman Dr. Huntsville, AL 35805, USA), AK(Department of Physics, The George Washington University, Washington, DC 20052, USA), AL(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AM(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA), AN(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA), AO(Physics Department, Boise State University, Boise, ID 83725, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 419, Issue 1, pp. 614-623. (MNRAS Homepage)
Publication Date:
01/2012
Origin:
WILEY
Astronomy Keywords:
gamma-ray burst: general
Abstract Copyright:
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
DOI:
10.1111/j.1365-2966.2011.19723.x
Bibliographic Code:
2012MNRAS.419..614U

Abstract

Spectral lag, which is defined as the difference in time of arrival of high- and low-energy photons, is a common feature in gamma-ray bursts (GRBs). Previous investigations have shown a correlation between this lag and the isotropic peak luminosity for long duration bursts. However, most of the previous investigations used lags extracted in the observer frame only. In this work (based on a sample of 43 Swift long GRBs with known redshifts), we present an analysis of the lag-luminosity relation in the GRB source frame. Our analysis indicates a higher degree of correlation -0.82 ± 0.05 (chance probability of ˜5.5 × 10-5) between the spectral lag and the isotropic peak luminosity, Liso, with a best-fitting power-law index of -1.2 ± 0.2, such that Liso ∝ lag-1.2. In addition, there is an anticorrelation between the source-frame spectral lag and the source-frame peak energy of the burst spectrum, Epk(1 + z).
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星期五, 八月 05, 2011

Bosnjak 2011 用磁化喷流解释高能光子的延迟

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Title:
Magnetic jet model for GRBs and the delayed arrival of >100 MeV photons
Authors:
Bosnjak, Z.; Kumar, P.
Publication:
eprint arXiv:1108.0929
Publication Date:
08/2011
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
5 pages; submitted to MNRAS
Bibliographic Code:
2011arXiv1108.0929B

Abstract

Photons of energy larger than 100 MeV from long-GRBs arrive a few seconds after <10 MeV photons do. We show that this delay is a natural consequence of a magnetic dominated relativistic jet. The much slower acceleration of a magnetic jet with radius (compared with a hot baryonic outflow) results in high energy gamma-ray photons to be converted to electron-positron pairs out to a larger radius whereas lower energy gamma-rays of energy less than ~10 MeV can escape when the jet crosses the Thomson-photosphere. The resulting delay for the arrival of high energy photons is found to be similar to the value observed by the Fermi satellite for a number of GRBs. A prediction of this model is that the delay should increase with photon energy (E) as E^{0.17} for E>100 MeV. The delay depends almost linearly on burst redshift, and on the distance from the central compact object where the jet is launched (R_0). Therefore, the delay in arrival of >10^2 MeV photons can be used to estimate burst redshift if the magnetic jet model for gamma-ray generation is correct and R_0 is roughly the same for long-GRBs.
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星期五, 十月 22, 2010

Shao, Lijing 2009 用去掉内在的time lag后的时延来限制 Lorentz violation

主要内容:
问题是他怎么知道哪些是内在的呢?

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Title:
Lorentz violation from cosmological objects with very high energy photon emissions
Authors:
Shao, Lijing; Xiao, Zhi; Ma, Bo-Qiang
Affiliation:
AA(School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China), AB(School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China), AC(School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China)
Publication:
Astroparticle Physics, Volume 33, Issue 5-6, p. 312-315. (APh Homepage)
Publication Date:
06/2010
Origin:
ELSEVIER
Abstract Copyright:
Elsevier B.V.
DOI:
10.1016/j.astropartphys.2010.03.003
Bibliographic Code:
2010APh....33..312S

Abstract

Lorentz violation (LV) is predicted by some quantum gravity theories, where photon dispersion relation is modified, and the speed of light becomes energy-dependent. Consequently, it results in a tiny time delay between high energy photons and low energy ones. Very high energy (VHE) photon emissions from cosmological distance can amplify these tiny LV effects into observable quantities. Here we analyze four VHE γ-ray bursts (GRBs) from Fermi observations, and briefly review the constraints from three TeV flares of active galactic nuclei (AGNs) as well. One step further, we present a first robust analysis of VHE GRBs taking the intrinsic time lag caused by sources into account, and give an estimate to quantum gravity energy ˜2×1017GeV for linear energy dependence, and ˜5×109GeV for quadratic dependence. However, the statistics is not sufficient due to the lack of data, and further observational results are desired to constrain LV effects better.
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星期四, 十月 21, 2010

Guiriec 2010 三个最亮和最硬的GBM短暴的时间分辨谱

主要内容:

GRB 090227B, GRB 090228  and GRB 090510

说他们的表现和长暴比较类似。


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Title:
Time-Resolved Spectroscopy of the 3 Brightest and Hardest Short Gamma-Ray Bursts Observed with the FGST Gamma-Ray Burst Monitor
Authors:
Guiriec, Sylvain; Briggs, Michael S.; Connaugthon, Valerie; Kara, Erin; Daigne, Frederic; Kouveliotou, Chryssa; van der Horst, Alexander J.; Paciesas, William; Meegan, Charles A.; Bhat, P. N.; Foley, Suzanne; Bissaldi, Elisabetta; Burgess, Michael; Chaplin, Vandiver; Diehl, Roland; Fishman, Gerald; Gibby, Melissa; Giles, Misty; Goldstein, Adam; Greiner, Jochen; Gruber, David; von Kienlin, Andreas; Kippen, Marc; McBreen, Sheila; Preece, Robert; Rau, Arne; Tierney, Dave; Wilson-Hodge, Colleen
Publication:
eprint arXiv:1009.5045
Publication Date:
09/2010
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics
Comment:
14 pages, 10 figures, 9 tables, Accepted for publication in the Astrophysical Journal September, 23 2010 (Submitted May, 16 2010) Corrections: 1 reference updated, figure 10 caption
Bibliographic Code:
2010arXiv1009.5045G

Abstract

From July 2008 to October 2009, the Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope (FGST) has detected 320 Gamma-Ray Bursts (GRBs). About 20% of these events are classified as short based on their T90 duration below 2 s. We present here for the first time time-resolved spectroscopy at timescales as short as 2 ms for the three brightest short GRBs observed with GBM. The time-integrated spectra of the events deviate from the Band function, indicating the existence of an additional spectral component, which can be fit by a power-law with index ~-1.5. The time-integrated Epeak values exceed 2 MeV for two of the bursts, and are well above the values observed in the brightest long GRBs. Their Epeak values and their low-energy power-law indices ({\alpha}) confirm that short GRBs are harder than long ones. We find that short GRBs are very similar to long ones, but with light curves contracted in time and with harder spectra stretched towards higher energies. In our time-resolved spectroscopy analysis, we find that the Epeak values range from a few tens of keV up to more than 6 MeV. In general, the hardness evolutions during the bursts follows their flux/intensity variations, similar to long bursts. However, we do not always see the Epeak leading the light-curve rises, and we confirm the zero/short average light-curve spectral lag below 1 MeV, already established for short GRBs. We also find that the time-resolved low-energy power-law indices of the Band function mostly violate the limits imposed by the synchrotron models for both slow and fast electron cooling and may require additional emission processes to explain the data. Finally, we interpreted these observations in the context of the current existing models and emission mechanisms for the prompt emission of GRBs.
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星期六, 九月 18, 2010

Arimoto 2010 HETE-II几个暴的时延关系统计

主要内容:

8 GRBs with known redshifts (GRB 010921, GRB
020124, GRB 020127, GRB 021211, GRB 030528, GRB 040924, GRB 041006, GRB 050408)



时延的关系和BATSE的暴一样,说明这个关系可以延伸到低能一些。(HETE-II比BATSE能段低。)

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Title:
Spectral-Lag Relations in GRB Pulses Detected with HETE-2
Authors:
Arimoto, Makoto; Kawai, Nobuyuki; Asano, Katsuaki; Hurley, Kevin; Suzuki, Motoko; Nakagawa, Yujin E.; Shimokawabe, Takashi; Pazmino, Nicolas Vasquez; Sato, Rie; Matsuoka, Masaru; Yoshida, Atsumasa; Tamagawa, Toru; Shirasaki, Yuji; Sugita, Satoshi; Takahashi, Ichiro; Atteia, Jean-Luc; Pelangeon, Alexandre; Vanderspek, Roland; Graziani, Carlo; Prigozhin, Gregory; Villasenor, Joel; Jernigan, J. Garrett; Crew, Geoffrey B.; Sakamoto, Takanori; Ricker, George R.; Woosley, Stanford E.; Butler, Nat; Levine, Alan; Doty, John P.; Donaghy, Timothy Q.; Lamb, Donald Q.; Fenimore, Edward; Galassi, Mark; Boer, Michel; Dezalay, Jean-Pascal; Olive, Jean-François; Braga, João; Manchanda, Ravi; Pizzichini, Graziella
Affiliation:
AA(Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551; arimoto@hp.phys.titech.ac.jp))
Publication:
Publications of the Astronomical Society of Japan, Vol.62, No.2, pp.487--499 (PASJ Homepage)
Publication Date:
04/2010
Origin:
PASJ
Keywords:
gamma rays: bursts, gamma rays: observations, radiation mechanisms: non-thermal
Bibliographic Code:
2010PASJ...62..487A

Abstract

Using a pulse-fit method, we investigated the spectral lags between the traditional gamma-ray band (50-400 keV) and the X-ray band (6-25 keV) for 8 GRBs with known redshifts (GRB 010921, GRB 020124, GRB 020127, GRB 021211, GRB 030528, GRB 040924, GRB 041006, and GRB 050408), detected with the WXM and FREGATE instruments aboard the HETE-2 satellite. We found several relations for individual GRB pulses between the spectral lag and other observables, such as the luminosity, pulse duration, and peak energy, Epeak. The obtained results are consistent with those for BATSE, indicating that the BATSE correlations are still valid at lower energies (6-25 keV). Furthermore, we found that the photon energy dependence for the spectral lags can be reconciled with the simple curvature effect model. We discuss the implications of these results from various points of view.
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星期五, 九月 17, 2010

Bednarz 2010 伽马暴时延的激波加速解释

主要内容:
说正的时延来自反射过程,负的时延来自Cracow加速过程。

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Title:
Relativistic slowing down shocks as sources of GRB lag
Authors:
Bednarz, Janusz
Publication:
eprint arXiv:1009.3100
Publication Date:
09/2010
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
extended work will be applied to ApJ
Bibliographic Code:
2010arXiv1009.3100B

Abstract

We are demonstrating in what way slowing down ultrarelativistic shocks are creating GRB lags. The reflection process produces positive lags and Cracow acceleration process negative lags. We present a way the seed particles are injected into relativistic jets.
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星期四, 八月 26, 2010

Ukwatta, T. N. 2010 暴源系中的时延-光度统计关系

主要内容:
有红移,对Swift暴做的,100-200keV和300-400keV(但BAT不是这个波段呀?)

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Title:
The lag-luminosity relation in the gamma-ray burst source-frame
Authors:
Ukwatta, T. N.; Dhuga, K. S.; Stamatikos, M.; Sakamoto, T.; Parke, W. C.; Barthelmy, S. D.; Gehrels, N.
Publication:
eprint arXiv:1003.0229
Publication Date:
02/2010
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
Accepted to be published in the Proceedings of "The Shocking Universe - Gamma-Ray Bursts and High Energy Shock Phenomena", Venice (Italy), September 14-18, 2009
Bibliographic Code:
2010arXiv1003.0229U

Abstract

We have investigated the empirical lag-luminosity relation in the Gamma-ray Burst (GRB) source-frame. We selected two energy bands (100-200 keV and 300-400 keV) in the GRB source-frame, which after redshift correction, lie in the observer-frame energy range of the Swift Burst Alert Telescope (BAT). The spectral lags between these energy channels are then presented as a function of the isotropic peak luminosity of the GRBs in the sample.
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星期二, 八月 24, 2010

Margutti, R. 2010 x射线耀发和伽马暴都满足L_P-t_lag的关系

主要内容:
都满足L~1/T_lag,说明暴和XRFs同源。
还做了很多别的量的统计。

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Title:
Lag-luminosity relation in γ-ray burst X-ray flares: a direct link to the prompt emission
Authors:
Margutti, R.; Guidorzi, C.; Chincarini, G.; Bernardini, M. G.; Genet, F.; Mao, J.; Pasotti, F.
Affiliation:
AA(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy; Physics Department, University of Milano Bicocca, Piazza della Scienza 3, Milano 20126, Italy), AB(Physics Department, University of Ferrara, via Saragat 1, I-44122 Ferarra, Italy), AC(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy; Physics Department, University of Milano Bicocca, Piazza della Scienza 3, Milano 20126, Italy), AD(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AE(Racah Institute of Physics, Hebrew University of Jerusalem, Israel), AF(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AG(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 406, Issue 4, pp. 2149-2167. (MNRAS Homepage)
Publication Date:
08/2010
Origin:
WILEY
MNRAS Keywords:
radiation mechanisms: non-thermal, gamma-ray burst: general
Abstract Copyright:
(c) Journal compilation © 2010 RAS
DOI:
10.1111/j.1365-2966.2010.16824.x
Bibliographic Code:
2010MNRAS.406.2149M

Abstract

ABSTRACT The temporal and spectral analysis of nine bright X-ray flares out of a sample of 113 flares observed by Swift reveals that the flare phenomenology is strictly analogous to the prompt γ-ray emission: high-energy flare profiles rise faster, decay faster and peak before the low-energy emission. However, flares and prompt pulses differ in one crucial aspect: flares evolve with time. As time proceeds, flares become wider, with larger peak lag, lower luminosities and softer emission. The flare spectral peak energy Ep,i evolves to lower values following an exponential decay which tracks the decay of the flare flux. The two flares with best statistics show higher than expected isotropic energy Eiso and peak luminosity Lp,iso when compared to the Ep,i-Eiso and Ep,i-Liso prompt correlations. Ep,i is found to correlate with Liso within single flares, giving rise to a time-resolved Ep,i(t)-Liso(t). Like prompt pulses, flares define a lag-luminosity relation: L0.3-10keVp,iso ~ t-0.95+/-0.23lag. The lag-luminosity is proven to be a fundamental law extending ~5 decades in time and ~5 decades in energy. Moreover, this is direct evidence that γ-ray burst (GRB) X-ray flares and prompt γ-ray pulses are produced by the same mechanism. Finally we establish a flare-afterglow morphology connection: flares are preferentially detected superimposed to one-break or canonical X-ray afterglows.

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Title:
Lag-luminosity relation in gamma-ray burst X-ray flares
Authors:
Margutti, R.
Publication:
eprint arXiv:1006.4103
Publication Date:
06/2010
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
To appear in: "Deciphering the ancient universe with GRBs", Kyoto 2010, conference proceeding
Bibliographic Code:
2010arXiv1006.4103M

Abstract

In strict analogy to prompt pulses, X-ray flares observed by Swift-XRT in long Gamma-Ray Bursts define a lag-luminosity relation: L_p,iso \propto t_lag^{-0.95+/-0.23}. The lag-luminosity is proven to be a fundamental law extending 5 decades in time and 5 in energy. This is direct evidence that GRB X-ray flares and prompt gamma-ray pulses are produced by the same mechanism.

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星期日, 八月 22, 2010

Misra, Ranjeev 2010 解析估计时延的误差

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Title:
Analytical error estimate for the cross-correlation, phase and time lag between two light curves
Authors:
Misra, Ranjeev; Bora, Archana; Dewangan, Gulab
Publication:
eprint arXiv:1006.4069
Publication Date:
06/2010
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
Submitted to MNRAS
Bibliographic Code:
2010arXiv1006.4069M

Abstract

Temporal analysis of radiation from Astrophysical sources like Active Galactic Nuclei, X-ray Binaries and Gamma-ray bursts provide information on the geometry and sizes of the emitting regions. Robustly establishing that two light-curves in different energy bands are correlated and measuring the phase and time-lag between them is an important and frequently used temporal diagnostic. Analytical expressions to estimate the errors on the cross-correlation, phase and time-lag between two light-curves are presented. Earlier estimates depended upon numerically expensive simulations or on dividing the light-curves in large number of segments to find the variance. Thus, the analytical estimates presented here allow for analysis of light-curves with relatively small (~ 1000) number of points, as well as to obtain information on the longest time-scales available. The error estimation is verified using simulations of light-curves derived from both white and 1/f stochastic processes with measurement errors. As a demonstration, we apply this technique to the XMM-Newton light-curves of the Active Galactic Nucleus, Akn 564.
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Margutti, R. 2010 x射线耀发和伽马暴都满足L_P-t_lag的关系

主要内容:
大致为L_P~1/T_lag
说明X射线耀发和暴本身的相同起源。

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Title:
Lag-luminosity relation in gamma-ray burst X-ray flares
Authors:
Margutti, R.
Publication:
eprint arXiv:1006.4103
Publication Date:
06/2010
Origin:
ARXIV
Keywords:
Astrophysics - High Energy Astrophysical Phenomena
Comment:
To appear in: "Deciphering the ancient universe with GRBs", Kyoto 2010, conference proceeding
Bibliographic Code:
2010arXiv1006.4103M

Abstract

In strict analogy to prompt pulses, X-ray flares observed by Swift-XRT in long Gamma-Ray Bursts define a lag-luminosity relation: L_p,iso \propto t_lag^{-0.95+/-0.23}. The lag-luminosity is proven to be a fundamental law extending 5 decades in time and 5 in energy. This is direct evidence that GRB X-ray flares and prompt gamma-ray pulses are produced by the same mechanism.
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