Magnetar giant flare high-energy emission

被引：1

作者：

Elenbaas, C. ^{[1
]}

Huppenkothen, D. ^{[2
,3
]}

Omand, C. ^{[4
,5
]}

Watts, A. L. ^{[1
]}

Bissaldi, E. ^{[6
,7
]}

Caiazzo, I. ^{[4
]}

Heyl, J. ^{[4
]}

机构：

[1] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[2] NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA

[3] NYU, Ctr Data Sci, 65 5th Ave,7th Floor, New York, NY 10003 USA

[4] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada

[5] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1138656, Japan

[6] Politecn Bari, Dipartimento Interateneo Fis, Via E Orabona 4, I-70125 Bari, Italy

[7] INFN, Sez Bari, Via E Orabona 4, I-70125 Bari, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 471卷 / 02期

基金：

加拿大自然科学与工程研究理事会;

关键词：

magnetic fields; radiation mechanisms: non-thermal; scattering; stars: magnetars; GAMMA-RAY BURST; 2004; DECEMBER; 27; SGR 1900+14; RADIATIVE MECHANISM; INTEGRAL DISCOVERY; 4U 0142+61; SOFT; PERSISTENT; SIMULATIONS; SGR-1806-20;

D O I：

10.1093/mnras/stx1727

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

High-energy (>250 keV) emission has been detected persisting for several tens of seconds after the initial spike of magnetar giant flares (GFs). It has been conjectured that this emission might arise via inverse Compton scattering in a highly extended corona generated by super-Eddington outflows high up in the magnetosphere. In this paper, we undertake a detailed examination of this model. We investigate the properties of the required scatterers, and whether themechanism is consistent with the degree of pulsed emission observed in the tail of the GF. We conclude that the mechanism is consistent with current data, although the origin of the scattering population remains an open question. We propose an alternative picture in which the emission is closer to that star and is dominated by synchrotron radiation. The Reuven Ramaty High Energy Solar Spectroscopic Imager observations of the 2004 December flare modestly favour this latter picture. We assess the prospects for the Fermi Gamma-ray Space Telescope to detect and characterize a similar high-energy component in a future GF. Such a detection should help to resolve some of the outstanding issues.

引用

页码：1856 / 1872

页数：17

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