Open AccessThe outburst radial velocity curve of X‐ray Nova Scorpii 1994 (= GRO J1655−40): a reduced mass for the black hole?
Author(s) -
Phillips S. N.,
Shahbaz T.,
Podsiadlowski Ph.
Publication year - 1999
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1999.02357.x
Subject(s) - physics , astrophysics , nova (rocket) , radial velocity , neutron star , black hole (networking) , x ray binary , supernova , stellar black hole , astronomy , stars , galaxy , aeronautics , engineering , computer network , routing protocol , routing (electronic design automation) , computer science , link state routing protocol
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.