An evolutionary scenario for short-period millisecond binary pulsars

Details An evolutionary scenario for short-period millisecond binary pulsars An evolutionary scenario for short-period millisecond binary pulsars

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.280.1000e&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 280, Issue 4, pp. 1000-1006.

Astronomy and Astrophysics

Astronomy

17

Binaries: Close, Stars: Evolution, Pulsars: General, Pulsars: Individual: Psr J1744-24A, Pulsars: Individual: Psr J0751+18, Pulsars: Individual: Psr J1012+5307

Scientific paper

We present numerical calculations that simulate the evolution of a low-mass (1-M_) star transferring mass to a compact object. Mass transfer starts when the low-mass star (secondary) turns off the main sequence (having a small helium core). We have calculated five evolutionary sequences with the assumption of non-conservative evolution and one sequence with conservative evolution. We can conclude that near the bifurcation point the evolution is very sensitive to: (i) the assumption of conservative or non-conservative evolution; (ii) the structure of the mass-losing star. Small changes in the initial period when the secondary fills its Roche lobe will lead to large changes in the final period and mass of the remnant. Our calculations support the model of Kluzniak, Czerny & Ray in which the secondary star of PSR 1744-24A fills its Roche lobe when it turns off the main sequence. Owing to the low accretion rate the system is in the `propeller' phase which may explain its very erratic eclipsing behaviour. The orbital parameters of PSR J0751+18 may be explained if we assume non-conservative evolution starting from an initial period (P_i) of 1.05d. After the accretion stops near 0.343d the system will evolve because of gravitational wave radiation (GWR), and after ~7.5x10^9 yr its orbital parameters will be as observed. We can explain the orbital parameters of PSR J1012+5307 if we again assume non-conservative evolution but this time starting with an initial period between 0.53 and 0.63d. Since the orbital period is relatively large, GWR is ineffective, and the orbital period of the system will be as it was when the system detached.

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