New insight into the origin of the GeV flare in the binary system PSR B1259-63/LS 2883 from the 2017 periastron passage

被引：20

作者：

Chernyakova, M. ^{[1
,2
,3
]}

Malyshev, D. ^{[4
]}

Mc Keague, S. ^{[1
,2
]}

van Soelen, B. ^{[5
]}

Marais, J. P. ^{[5
]}

Martin-Carrillo, A. ^{[6
]}

Murphy, D. ^{[6
]}

机构：

[1] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland

[2] Dublin City Univ, CfAR, Dublin 9, Ireland

[3] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland

[4] Univ Tubingen, Inst Astron & Astrophys Tubingen, Sand 1, D-72076 Tubingen, Germany

[5] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa

[6] Univ Coll Dublin, Sch Phys, Space Sci Grp, Dublin 4, Ireland

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 497卷 / 01期

基金：

爱尔兰科学基金会;

关键词：

gamma rays: general; pulsars: individual: PSR B1259-63; stars:; emission-line; Be; X-rays: binaries; X-rays: individual: PSR B1259-63; radiation mechanisms: non-thermal; MULTIWAVELENGTH OBSERVATIONS; PARTICLE-ACCELERATION; SHOCK ACCELERATION; COMPTON-SCATTERING; PULSAR; RADIO; EMISSION; RAYS; DISC;

D O I：

10.1093/mnras/staa1876

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbiting around an O9.5Ve star, LS 2883, with a period of similar to 3.4 yr. The interaction of the pulsar wind with the LS 2883 outflow leads to unpulsed broad-band emission in the radio, X-rays, GeV, and TeV domains. While the radio, X-ray, and TeV light curves show rather similar behaviour, the GeV light curve appears very different with a huge outburst about a month after a periastron. The energy release during this outburst seems to significantly exceed the spin-down luminosity of the pulsar and both the GeV light curve and the energy release vary from one orbit to the next. In this paper, we present for the first time the results of optical observations of the system in 2017, and also reanalyse the available X-ray and GeV data. We present a new model in which the GeV data are explained as a combination of the bremsstrahlung and inverse Compton emission from the unshocked and weakly shocked electrons of the pulsar wind. The X-ray and TeV emission is produced by synchrotron and inverse Compton emission of energetic electrons accelerated on a strong shock arising due to stellar/pulsar winds collision. The brightness of the GeV flare is explained in our model as a beaming effect of the energy released in a cone oriented, during the time of the flare, in the direction of the observer.

引用

页码：648 / 655

页数：8

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