An Accretion Induced Collapse Model for the Eclipsing Binary Pulsar PSR:1718-19

Details An Accretion Induced Collapse Model for the Eclipsing Binary Pulsar PSR:1718-19 An Accretion Induced Collapse Model for the Eclipsing Binary Pulsar PSR:1718-19

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...273l..38e&link_type=abstract

Astronomy and Astrophysics, Vol.273, NO. 1/JUNI, P. L38, 1993

Astronomy and Astrophysics

Astrophysics

14

Eclipsing Binary Pulsar, Psr1718-19, Accretion Induced Collapse

Scientific paper

A possible model for the recently discovered pulsar PSR1718-19 (Lyne et al.,1993) in the globular cluster NGC 6342 is discussed. This is a 6.2 hour eclipsing binary system with rotational period of 1 s and magnetic field of ≍ 1012 G. It is proposed that this system has been formed by the accretion induced collapse of a massive white dwarf about 107 yr ago. Three stages of thermal evolution of the secondary are proposed: 1. Before the collapse the when white dwarf is very near to the Chandrasekhar limit and its X-ray luminosity may be more than 1033 erg/s. Due to the short orbital separation (a ≍ (4-6) 1010 cm) the flux at the surface of companion will be more than 1010 erg/scm2. If such a heating occurs during several hundred Myr then the secondary will strongly expand and violent mass transfer starts. 2. During the first 105 yr after the collapse the companion of the newly formed rapidly rotating neutron star is in the intensive pulsar radiation field with Lp 4 × 1036 erg/s and will remain out of thermal equilibrium. 3. After the pulsar spin-down to its current rotational period the pulsar action will switch off. Since the thermal timescale of the companion is much longer (≍ 100 Myr) than than system timescale (≍ 10 Myr) the Roche lobe overflow from the companion may be a source of material in the system. AM Her systems EXO 033319-2554.2 and RE2107-05 could be possible progenitors of such a system.

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