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Transition from Fireball to Poynting-flux-dominated Outflow in Three-Episode GRB 160625B

B.-B. ZhangB. ZhangA. J. Castro‐TiradoInstituto de Astrofísica de Andalucía (IAA-CSIC) , P.O. Box 03004 , E-18080 Granada , Spain;Z. G. DaiKey laboratory of Modern Astron. Astrophys. ( Nanjing University) , Ministry of Education , Nanjing 210093 , China;P. H. T. TamSchool of Physics and Astronomy , Sun Yat-Sen University , Zhuhai 519082 , China;X.-Y. WangKey laboratory of Modern Astron. Astrophys. ( Nanjing University) , Ministry of Education , Nanjing 210093 , China;Y. D. HuInstituto de Astrofísica de Andalucía (IAA-CSIC) , P.O. Box 03004 , E-18080 Granada , Spain;С. КарповKazan Federal University , Kazan , Russia;A. PozanenkoF.-W. ZhangCollege of Science , Guilin University of Technology , Guilin 541004 , China;E. MazaevaSpace Research Institute of the Russian Academy of Sciences , 117997 , Rus- sia , Moscow , Profsoyuzanaya , 84/32 ;P. Yu. MinaevSpace Research Institute of the Russian Academy of Sciences , 117997 , Rus- sia , Moscow , Profsoyuzanaya , 84/32 ;A. VolnovaSpace Research Institute of the Russian Academy of Sciences , 117997 , Rus- sia , Moscow , Profsoyuzanaya , 84/32 ;S. R. OatesDepartment of Physics , University of Warwick , Coventry , CV4 7AL , UK;He GaoDepartment of Astronomy , Beijing Normal University , Beijing 100875 , China;Xue-Feng WuL. ShaoPurple Mountain Observatory , Chinese Academy of Sciences , Nanjing 210008 , China;Qing-Wen TangDepartment of Physics , Nanchang University , Nanchang 330031 , China;Grigory M. BeskinKazan Federal University , Kazan , Russia;A. BiryukovKazan Federal University , Kazan , Russia;S. BondarResearch and Production Corporation "Precision Systems and Instruments" , Nizhniy Arkhyz , Russia;E. IvanovResearch and Production Corporation "Precision Systems and Instruments" , Nizhniy Arkhyz , Russia;E. KatkovaResearch and Production Corporation "Precision Systems and Instruments" , Nizhniy Arkhyz , Russia;Orekhova, N.Research and Production Corporation "Precision Systems and Instruments" , Nizhniy Arkhyz , Russia;A. PerkovResearch and Production Corporation "Precision Systems and Instruments" , Nizhniy Arkhyz , Russia;Vyacheslav V. SasyukKazan Federal University , Kazan , Russia;L. MankiewiczCenter for Theoretical Physics PAS , Al. Lotnikow 32/46 , 02-668 Warsaw , Poland;A. F. ŻarneckiFaculty of Physics , University of Warsaw , Pasteura 5 , 02-093 Warsaw , Poland;A. ĆwiekNational Centre for Nuclear Research , Hoża 69 , 00-681 Warsaw , Poland;Rafał OpielaCenter for Theoretical Physics PAS , Al. Lotnikow 32/46 , 02-668 Warsaw , Poland;A. ZadrożnyNational Centre for Nuclear Research , Hoża 69 , 00-681 Warsaw , Poland;R. AptekarIoffe Institue , Politekhnicheskaya ul. , 26, St. Petersburg , 194021 , Russia;D. FrederiksIoffe Institue , Politekhnicheskaya ul. , 26, St. Petersburg , 194021 , Russia;D. SvinkinIoffe Institue , Politekhnicheskaya ul. , 26, St. Petersburg , 194021 , Russia;A. V. KusakinFesenkov Astrophysical Institute , Kazakhstan , Almaty , 050020 , 23 ;R. Inasaridze;О. БурхоновUlugh Beg Astronomical Institute , Uzbekistan , 100052 , Tashkent , Astronomicheskaya st ., 33 ;V. RumyantsevCrimean Astrophysical Observatory , 298409 , Nauchny , Crimea;Evgeny KlunkoInstitute of Solar-Terrestrial Physics , 664033 , Russia , Irkutsk p/ o box 291 ; Lermontov st ., 126aА. С. МосквитинSpecial Astrophysical Observatory of Russian Academy of Sciences , Nizhniy Arkhyz , Russia;Timur A. FatkhullinSpecial Astrophysical Observatory of Russian Academy of Sciences , Nizhniy Arkhyz , Russia;В. В. СоколовSpecial Astrophysical Observatory of Russian Academy of Sciences , Nizhniy Arkhyz , Russia;A. F. ValeevKazan Federal University , Kazan , Russia;S. JeongDepartment of Physics , Sungkyunkwan Uni- versity (SKKU) , Suwon , 440-746 Korea;I. H. ParkDepartment of Physics , Sungkyunkwan Uni- versity (SKKU) , Suwon , 440-746 Korea;M. D. Caballero‐GarcíaR. CunniffeInstituto de Astrofísica de Andalucía (IAA-CSIC) , P.O. Box 03004 , E-18080 Granada , Spain;J. C. TelloInstituto de Astrofísica de Andalucía (IAA-CSIC) , P.O. Box 03004 , E-18080 Granada , Spain;P. FerreroInstituto de Astrofísica de Andalucía (IAA-CSIC) , P.O. Box 03004 , E-18080 Granada , Spain;S. B. PandeyARIES , Manora Peak , Nainital , India; 38 School of Physics and Electronic Science, Guizhou Normal Univer- sity, Guiyang, Guizhou 550001, People's Republic of China; 39 Departamento de Algebra, Geometría y Topología, Facultad de Ciencias, Universidad de Málaga, C. Juan López Peñalver, sn, 29071 Málaga, SpainM. JelínekAstronomical Institute of the Academy of Sciences , Bocni II 1401 , CZ-141 00 PrahaFang‐Kun PengSchool of Physics , Peking University , Beijing 100871 , China;R. Sánchez-RamírezInstituto de Astrofísica de Andalucía (IAA-CSIC) , P.O. Box 03004 , E-18080 Granada , Spain;A. CastellónSchool of Physics , Peking University , Beijing 100871 , China;

2016en

Ochiq kirishYashil

ABI

Annotatsiya

The ejecta composition is an open question in gamma-ray bursts (GRB) physics. Some GRBs possess a quasi-thermal spectral component in the time-resolved spectral analysis, suggesting a hot fireball origin. Others show a featureless non-thermal spectrum known as the "Band" function, consistent with a synchrotron radiation origin and suggesting that the jet is Poynting-flux-dominated at the central engine and likely in the emission region as well. There are also bursts showing a sub-dominant thermal component and a dominant synchrotron component suggesting a likely hybrid jet composition. Here we report an extraordinarily bright GRB 160625B, simultaneously observed in gamma-rays and optical wavelengths, whose prompt emission consists of three isolated episodes separated by long quiescent intervals, with the durations of each "sub-burst" being $\sim$ 0.8 s, 35 s, and 212 s, respectively. Its high brightness (with isotropic peak luminosity L$_{\rm p, iso}\sim 4\times 10^{53}$ erg/s) allows us to conduct detailed time-resolved spectral analysis in each episode, from precursor to main burst and to extended emission. The spectral properties of the first two sub-bursts are distinctly different, allowing us to observe the transition from thermal to non-thermal radiation between well-separated emission episodes within a single GRB. Such a transition is a clear indication of the change of jet composition from a fireball to a Poynting-flux-dominated jet.

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Identifikatorlar

DOI: 10.48550/arxiv.1612.03089

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