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2001ApJ...546..455D - Astrophys. J., 546, 455-468 (2001/January-1)
The orbit of X Persei and its neutron star companion.
DELGADO-MARTI H., LEVINE A.M., PFAHL E. and RAPPAPORT S.A.
Abstract (from CDS):
We discuss the formation of the system in the context of the standard evolutionary scenario for Be/X-ray binaries. We find that the system most likely formed from a pair of massive progenitor stars and probably involved a quasi-stable and nearly conservative transfer of mass from the primary to the secondary. We find that the He star remnant of the primary most likely had a mass ≲6 M☉ after mass transfer. If the supernova explosion was completely symmetric, then the present orbital eccentricity indicates that ≲4 M☉ was ejected from the binary. If, on the other hand, the neutron star received at birth a ``kick'' of the type often inferred from the velocity distribution of isolated radio pulsars, then the resultant orbital eccentricity would likely have been substantially larger than 0.11. We have carried out a Monte Carlo study of the effects of such natal kicks and find that there is less than a 1% probability of a system like that of X Per forming with an orbital eccentricity e≲0.11. We speculate that there may be a substantial population of neutron stars formed with little or no kick. Finally, we discuss the connected topics of the wide orbit and accretion by the neutron star from a stellar wind.
Abstract Copyright: ∼
Journal keyword(s): Stars: Individual: Constellation Name: X Persei - Stars: Individual: Alphanumeric: 4U 0352+30 - Stars: Neutron - Stars: Supernovae: General - X-Rays: Stars
Simbad objects: 8
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