The outburst radial velocity curve of X-ray Nova Scorpii 1994 (= GRO J1655-40): a reduced mass for the black hole?

被引：34

作者：

Phillips, SN ^{[1
]}

Shahbaz, T ^{[1
]}

Podsiadlowski, P ^{[1
]}

机构：

[1] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 1999年 / 304卷 / 04期

关键词：

accretion; accretion discs; binaries : close; stars : individual : X-ray Nova Sco 1994 (GRO J1655-40); X-rays : stars;

D O I：

10.1046/j.1365-8711.1999.02357.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a re-analysis of the outburst radial velocity data for X-ray Nova Scorpii 1994. Using a model based on X-ray heating of the secondary star, we suggest a more realistic treatment of the radial velocity data. Solutions are obtained in the (K-2,q) plane which, when combined with the published value for the binary mass ratio and inclination, constrain the mass of the black hole to within the region 4.1 < M-1 < 6.6 M-. (90 per cent confidence), which is significantly lower than the value obtained by Orosz & Bailyn, This reduced lower bound for the black hole mass, together with the high space velocity of the system, is consistent with the idea that it was formed by the post-supernova collapse of a neutron star.

引用

页码：839 / 844

页数：6

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