Massive X-ray binaries - Their physics and evolution

Details Massive X-ray binaries - Their physics and evolution Massive X-ray binaries - Their physics and evolution

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.118..257s&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Physics

Pulsars, Stellar Evolution, Stellar Physics, Supermassive Stars, X Ray Binaries, Neutron Stars, Stellar Envelopes, Stellar Magnetic Fields, Stellar Mass Accretion, Stellar Orbits, Stellar Rotation, Stellar Winds, Supernovae

Scientific paper

In the expectation that moderately massive close binaries evolve into Be X-ray binaries, while very massive systems evolve into standard X-ray binaries, attention is given to various aspects of massive X-ray binaries. After an initial supernova explosion, tidal forces circularize the orbit of short period systems; the expansion of the optical star over the course of its evolution will continuously disturb the stability of the orbit. Short period systems with large mass ratio may eventually become tidally unstable. A method for the representation of the rotational and magnetic evolution of neutron stars in close binary systems is presented, and it is suggested that while such fast X-ray pulsars as 4U 0115 + 63 are young neutron stars, Cen X-3 and SMC X-1 are 'recycled' pulsars.

Affiliated with

Also associated with

No associations

Rating

Massive X-ray binaries - Their physics and evolution does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Massive X-ray binaries - Their physics and evolution, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Massive X-ray binaries - Their physics and evolution will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1844118