Close Encounters between a Neutron Star and a Main-Sequence Star

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dc.creatorLee, Hyung Mok
dc.creatorKim, Sungsoo S.
dc.creatorKang, Hyesung
dc.date1996-03-27
dc.date.accessioned2026-07-07T02:21:03Z
dc.date.available2026-07-07T02:21:03Z
dc.descriptionWe have examined consequences of strong tidal encounters between a neutron star and a normal star using SPH as a possible formation mechanism of isolated recycled pulsars in globular clusters. We have made a number of SPH simulations for close encounters between a main-sequence star of mass ranging from 0.2 to 0.7 Solar masses represented by an n=3/2 polytrope and a neutron star represented by a point mass. The outcomes of the first encounters are found to be dependent only on the dimensionless parameter eta' = (m/(m+M))^(1/2) (r_min/R_MS)^(3/2) (m/M)^(1/6), where m and M are the masses of the main-sequence star and the neutron star, respectively, r_min the minimum separation between two stars, and R_MS the size of the main-sequence star. The material from the (at least partially) disrupted star forms a disk around the neutron star. If all material in the disk is to be acctreted onto the neutron star's surface, the mass of the disk is enough to spin up the neutron star to spin period of 1 ms.
dc.description13 pages with 7 Figures. Tarred, gzipped, uuencoded LaTeX file. Complete Figures available at http://mercury.es.pusan.ac.kr/papers.html (381kb). To appear in the Journal of the Korean Astronomical Society
dc.identifierhttps://arxiv.org/abs/astro-ph/9603137
dc.identifierhttp://arxiv.org/abs/astro-ph/9603137
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/10415
dc.subjectAstrophysics
dc.titleClose Encounters between a Neutron Star and a Main-Sequence Star
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