The Evolution of Relativistic Binary Progenitor Systems

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Abstract
Relativistic binary pulsars, such as B1534+12 and B1913+16, are characterized by having close orbits with a binary separation of ~3 R☉. The progenitor of such a system is a neutron star, helium star binary. The helium star, with a strong stellar wind, is able to spin up its compact companion via accretion. The neutron star's magnetic field is then lowered to observed values of about ~1010 G. Since the pulsar lifetime is inversely proportional to its magnetic field, the possibility of observing such a system is thus enhanced by this type of evolution. We will show that a nascent (Crab-like) pulsar in such a system can, through accretion-braking torques (i.e., the "propeller effect") and wind-induced spin-up rates, reach periods that are close to observed values. Such processes occur within the relatively short helium star lifetimes. Additionally, we find that the final outcome of such evolutionary scenarios depends strongly on initial parameters, particularly the initial binary separation and helium star mass. Indeed, the majority of such systems end up in the pulsar "graveyard," and only a small fraction are strongly recycled. This fact might help to reconcile theoretically expected birth rates with limited observations of relativistic binary pulsars.
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