Abstract
Recent data on low-mass X-ray binaries (LMXBs) and msec pulsars (MSPs) pose a challenge to evolutionary theories which neglect the effects of disk and companion irradiation. Here we discuss the main features of a radiation-driven (RD) evolutionary model that may be applicable to several LMXBs. According to this model, radiation from the accreting compact star in LMXBs ‘vaporizes’ the accretion disk and the companion star by driving a self-sustained mass loss until a sudden accretion-turn off occurs. The main characteristics of the RD-evolution are: (1) the lifetime of RD-LMXB’s is of order 107 years or less; (2) both the orbital period gap and the X-ray luminosity may be consequences of RD-evolution of LMXB’s containing lower main sequence and degenerate companion stars; (3) the companion star may transfer mass to the primary even if it underfills its Roche lobe; (4) the recycled msec pulsar can continue to vaporize the low-mass companion star even after the accretion turn-off produced by a strong pulsar wind; (5) the RD-evolutionary model resolves the apparent statistical discrepancy between the number of MSP’s and their LMXB progenitors.
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Heraclitus
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Tavani, M. (1991). Vaporizing Neutron Stars in Low-Mass X-Ray Binaries and the Statistics of Millisecond Pulsars. In: Ventura, J., Pines, D. (eds) Neutron Stars: Theory and Observation. NATO ASI Series, vol 344. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-3536-8_12
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DOI: https://doi.org/10.1007/978-94-011-3536-8_12
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