Formation of a single millisecond pulsar by the coalescence of a neutron star and a massive white dwarf

Details Formation of a single millisecond pulsar by the coalescence of a neutron star and a massive white dwarf Formation of a single millisecond pulsar by the coalescence of a neutron star and a massive white dwarf

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139l..16v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 1, Oct. 1984, p. L16-L18.

Astronomy and Astrophysics

Astrophysics

35

Binary Stars, Gravitational Waves, Pulsars, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, Accretion Disks, Neutron Stars, Orbit Decay, Radii, Roche Limit, Stellar Mass, Stellar Models

Scientific paper

It is shown that a close binary (P < 16h) consisting of a neutron star and a massive white dwarf (M > 0.7 M_sun;) inevitably evolves towards coalescence as a consequence of gravitational radiation losses. The reason for coalescence into a single object is: the steep mass-radius relation of massive white dwarfs, which causes runaway mass transfer to ensue as soon as the white dwarf overflows its Roche lobe. The white dwarf is disrupted on its dynamical timescale (a few seconds). Part of its matter (≥ 0.10 M_sun;) is expected to be accreted by the neutron star through a disk. This provides a viable model for forming a single millisecond pulsar. As its progenitor system may have descended from a moderately massive (B-type) binary system with a low or moderate runaway velocity, such a pulsar may be expected to have a location close to the galactic plane, like the 1.5 msec pulsar.

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