Binary Evolution Leading to the Radio Pulsar PSR J1614-2230

Details Binary Evolution Leading to the Radio Pulsar PSR J1614-2230 Binary Evolution Leading to the Radio Pulsar PSR J1614-2230

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21743226l&link_type=abstract

American Astronomical Society, AAS Meeting #217, #432.26; Bulletin of the American Astronomical Society, Vol. 43, 2011

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We have computed an extensive grid of binary evolution tracks to represent low- and intermediate mass X-ray binaries (LMXBs and IMXBs). The grid includes 42,000 models which covers 60 initial donor masses over the range of 1-4 solar masses and, for each of these, 700 initial orbital periods over the range of 10-250 hours. These results can be applied to understanding LMXBs and IMXBs that evolve analogously to CVs; that form ultracompact binaries with orbital periods in the range of 6-50 minutes; and that lead to wide orbits with giant donors. We also investigate the relic binary recycled radio pulsars into which these systems evolve. To evolve the donor stars in this study, we utilized a newly developed stellar evolution code called "MESA" that was designed, among other things, to be able to handle very low-mass and degenerate donors. This first application of the results is aimed at an understanding of the newly discovered pulsar PSR J1614-2230 which has a 1.97 solar masses neutron star, orbital period = 8.7 days, and a companion star of 0.5 solar masses. We show that (i) this system is a cousin to the LMXB Cyg X-2, (ii) the initial donor star had a mass between 3.4-3.8 solar masses, (iii) neutron stars this massive are not easy to produce in spite of the initially high mass of the donor star, and (iv) the current companion star is largely composed of CO, but should have a surface H abundance of 15%.

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