The black hole in NGC 1313 X-2

被引：1

作者：

Zampieri, L. ^{[1
]}

Patruno, A. ^{[2
]}

机构：

[1] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[2] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands

来源：

ASTRONOMISCHE NACHRICHTEN | 2011年 / 332卷 / 04期

关键词：

accretion; accretion disks; black hole physics; galaxies: individual (NGC 1313); X-rays: binaries; X-rays: individuals (NGC 1313 X-2); X-RAY SOURCE; XMM-NEWTON OBSERVATIONS; SPIRAL GALAXY NGC-1313; RED GIANT BRANCH; METAL-POOR STARS; OPTICAL COUNTERPART; ORBITAL PERIOD; VARIABILITY; DISCOVERY; METALLICITY;

D O I：

10.1002/asna.201011513

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The amount of data available for NGC 1313 X-2 make it a cornerstone for the study of ultraluminous X-ray sources (ULXs). We modelled the optical and X-ray data of this ULX with a binary evolution code that takes into account X-ray irradiation. We restricted the candidate binary system to be either a 50-100 M-circle dot black hole (BH) accreting from a 12-15 M-circle dot main sequence star or a 20 M-circle dot BH with a 12-15 M-circle dot giant donor. If the orbital period of the system is similar to 6 days, a 20 M-circle dot BH model becomes unlikely and we are left with the only possibility that the compact accretor in NGC1313 X-2 is a massive BH of 50-100 M-circle dot. We briefly discuss these results within the framework of an alternative scenario for the formation of ULXs, in which a portion of them may contain BHs of >= 30-40 M-circle dot formed from very massive stars in a low metallicity environment. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim

引用

页码：422 / 425

页数：4

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