EDP Sciences
Free Access
Volume 370, Number 1, April IV 2001
Page(s) 170 - 175
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20010192
Published online 15 April 2001

A&A 370, 170-175 (2001)
DOI: 10.1051/0004-6361:20010192

The origin of the runaway high-mass X-ray binary HD 153919/4U1700-37

A. Ankay1, 2, L. Kaper1, J. H. J. de Bruijne3, J. Dewi1, R. Hoogerwerf3 and G. J. Savonije1

1  Astronomical Institute "Anton Pannekoek"and Center for High-Energy Astrophysics, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2  Middle East Technical University, Physics Department, 06531 Ankara, Turkey
3  Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands

(Received 8 September 2000 / Accepted 31 January 2001 )

Based on its Hipparcos proper motion, we propose that the high-mass X-ray binary HD 153919/4U1700-37 originates in the OB association Sco OB1. At a distance of 1.9 kpc the space velocity of 4U1700-37 with respect to Sco OB1 is 75 km s-1. This runaway velocity indicates that the progenitor of the compact X-ray source lost about 7 $M_{\odot}$ during the (assumed symmetric) supernova explosion. The system's kinematical age is about $2 \pm 0.5$ million years which marks the date of the supernova explosion forming the compact object. The present age of Sco OB1 is $\la$8 Myr; its suggested core, NGC 6231, seems to be somewhat younger (~5 Myr). If HD 153919/4U1700-37 was born as a member of Sco OB1, this implies that the initially most massive star in the system terminated its evolution within $\la$6 million years, corresponding to an initial mass $\ga$30 $M_{\odot}$. With these parameters the evolution of the binary system can be constrained.

Key words: stars: early type -- stars: mass loss -- stars: neutron -- stars: individual: HD 153919 -- 4U1700-37 -- ultraviolet: stars

Offprint request: L. Kaper, lexk@astro.uva.nl

SIMBAD Objects

© ESO 2001

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