Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...401..246d&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 401, no. 1, p. 246-259.
Astronomy and Astrophysics
Astrophysics
44
Binary Stars, Globular Clusters, Neutron Stars, Red Giant Stars, Stellar Evolution, Celestial Mechanics, Main Sequence Stars, Pulsars, Stellar Envelopes, X Ray Binaries
Scientific paper
Encounters between a 1.4 solar mass neutron star and a 0.8 solar mass red giant (RG) and between a 1.4 solar mass neutron star (NS) and an 0.8 solar mass main-sequence (MS) star have been successfully simulated. In the case of encounters involving an RG, bound systems are produced when the separation at periastron passage R(MIN) is less than about 2.5 R(RG). At least 70 percent of these bound systems are composed of the RG core and NS forming a binary engulfed in a common envelope of what remains of the former RG envelope. Once the envelope is ejected, a tight white dwarf-NS binary remains. For MS stars, encounters with NSs will produce bound systems when R(MIN) is less than about 3.5 R(MS). Some 50 percent of these systems will be single objects with the NS engulfed in a thick disk of gas almost as massive as the original MS star. The ultimate fate of such systems is unclear.
Benz Willy
Davies Melvyn B.
Hills Jack G.
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