Radio Ejection and the Orbital Period Gap in the Distribution of Wide Binary Millisecond Pulsars

Details Radio Ejection and the Orbital Period Gap in the Distribution of Wide Binary Millisecond Pulsars Radio Ejection and the Orbital Period Gap in the Distribution of Wide Binary Millisecond Pulsars

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..983..494n&link_type=abstract

40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP Conference Proceedings, Volume 983, pp. 494-496 (2008).

Computer Science

Pulsars, Neutron Stars, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, X-Ray Binaries

Scientific paper

We briefly review our current understanding of the various evolutionary channels that lead to the formation of wide Binary Millisecond Pulsars (bMSPs). Depending on the initial conditions at the onset of Roche lobe overflow, there is a very sharp bifurcation in the evolution of the orbital periods of these systems. Binary systems just below the bifurcation limit can evolve to become ultracompact systems (e.g., accretion-powered MSPs), while those above the limit will evolve to form bMSPs with periods of between approximately one day to 1000 days. One of the interesting features in the distribution of Galactic bMSPs is an orbital period gap of between ~20 and 60 days. We show that if the radio-ejection mechanism is efficient in preventing further accretion onto the spun-up neutron star, then the paucity of bMSPs in this period range can naturally be explained. The dependence of the orbital period distribution on the metallicity of the binary system is also investigated.

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