The binary pulsar PSRJ 2145-0750: A system originating from a low or intermediate mass X-ray binary with a donor star on the asymptotic giant branch?

Details The binary pulsar PSRJ 2145-0750: A system originating from a low or intermediate mass X-ray binary with a donor star on the asymptotic giant branch? The binary pulsar PSRJ 2145-0750: A system originating from a low or intermediate mass X-ray binary with a donor star on the asymptotic giant branch?

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...291l..39v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 291, no. 3, p. L39-L42

Astronomy and Astrophysics

Astrophysics

52

Asymptotic Giant Branch Stars, Pulsars, Stellar Envelopes, Stellar Evolution, Stellar Mass, X Ray Binaries, Mass Transfer, Stellar Magnetic Fields, Stellar Mass Accretion, Stellar Models, Stellar Orbits

Scientific paper

It is shown that the 6.84-day orbital period and relatively high companion mass of the 16.1ms period binary pulsar PSRJ 2145-0750 find a consistent explanantion if the progenitor-system consisted of a donor star in the mass range 1-6 solar mass with an orbital period such that this star overflowed its Roche-lobe on the Asymptotic Giant Branch (AGB). The present system then resulted after a phase of Common Envelope (CE) evolution. Initial donor masses in the range 2.4-6 solar mass are possible only if, in addition to the orbital gravitational binding energy, other energy sources are available for expelling the envelope. The post-CE remnants of donors in the mass range 4-6 solar mass overflow their Roche lobes and continue to transfer mass at a near or super Eddington rate for of order 106 yrs. This provides a simple way to explain the rapid spin and weak magnetic field of PSRJ 2145-0750.

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