Statistics – Computation
Scientific paper
Jul 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...318..760s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 318, July 15, 1987, p. 760-766.
Statistics
Computation
26
Globular Clusters, Main Sequence Stars, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, Computational Astrophysics, Neutron Stars, Stellar Cores, X Ray Binaries
Scientific paper
Collisions between a 0.2 solar mass main-sequence star and a white dwarf, in the core of a globular cluster, have been studied with the aid of a three-dimensional numerical simulation. For impact parameters between one and two main-sequence star radii (at an initial separation of five stellar radii), a massive disk forms around the white dwarf. Due to the non-Keplerian nature of the disks (i.e., significant internal pressure) formed in the present collision calculations, a definitive statement cannot be made concerning the final, stable configurations which result from such collisions. If, however, an accretion phase does follow the formation of massive disks, luminous X-ray (for neutron star accretors) and UV (for white dwarf accretors) sources can be expected to be formed this way in globular cluster cores.
Livio Mario
Regev Oded
Shara Michael M.
Soker Noam
No associations
LandOfFree
Massive disk formation resulting from the collision of a main-sequence star with a white dwarf in a globular cluster core 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 disk formation resulting from the collision of a main-sequence star with a white dwarf in a globular cluster core, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Massive disk formation resulting from the collision of a main-sequence star with a white dwarf in a globular cluster core will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-789772