X-ray binaries and their descendants: binary radio pulsars; evidence for three classes of neutron stars?
| dc.creator | Heuvel, E. P. J. van den | |
| dc.date | 2004-07-21 | |
| dc.date.accessioned | 2026-07-07T02:14:05Z | |
| dc.date.available | 2026-07-07T02:14:05Z | |
| dc.description | An important recent discovery by Pfahl et al. (2002) is that there are two classes of Be X-ray binaries: one with orbits of small eccentricity (<0.25), in which the neutron stars received hardly any kick velocity at birth and a class with substantial orbital eccentricities, in which the neutron stars received a kick velocity of order 100 km/s at birth. Also many of the double neutron stars (5 out of 7) have a low orbital eccentricity (0.09 to 0.27), which indicates that their second-born neutron stars received hardly any velocity kick at birth. These second-born neutron stars tend to have low masses (1.25 to 1.35 Msun). It is proposed that the low-mass, low-kick neutron stars are formed by the electron capture of degenerate O-Ne-Mg cores of stars with initial masses below about 12-14 Msun, while the high-kick neutron stars originated from the photo-disintegration collapse of the iron cores of stars which started out with masses larger than this limit. The latter group may be further subdivided into two classes of different mass. | |
| dc.description | 10 pages in pdf format; to appear in proceedings Fifth Integral Science Workshop | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0407451 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0407451 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/7982 | |
| dc.subject | Astrophysics | |
| dc.title | X-ray binaries and their descendants: binary radio pulsars; evidence for three classes of neutron stars? | |
| dc.type | text |