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arXiv · 1302.2492

A Metal-Rich Low-Gravity Companion to a Massive Millisecond Pulsar

David L. Kaplan·Varun B. Bhalerao·Marten H. van Kerkwijk·Detlev Koester·Shri R. Kulkarni·Kevin Stovall
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Abstract

Most millisecond pulsars with low-mass companions are in systems with either helium-core white dwarfs or non-degenerate ("black widow" or "redback") stars. A candidate counterpart to PSR J1816+4510 was identified by Kaplan et al. (2012) whose properties were suggestive of both types of companions although identical to neither. We have assembled optical spectroscopy of the candidate companion and confirm that it is part of the binary system with a radial velocity amplitude of 343+/-7 km/s, implying a high pulsar mass, Mpsr*sin^3i=1.84+/-0.11 Msun, and a companion mass Mc*sin^3i=0.192+/-0.012 Msun, where i is the inclination of the orbit. The companion appears similar to proto-white dwarfs/sdB stars, with a gravity log(g)=4.9+/-0.3, and effective temperature 16000+/-500 K. The strongest lines in the spectrum are from hydrogen, but numerous lines from helium, calcium, silicon, and magnesium are present as well, with implied abundances of roughly ten times solar (relative to hydrogen). As such, while from the spectrum the companion to PSR J1816+4510 is superficially most similar to a low-mass white dwarf, it has much lower gravity, is substantially larger, and shows substantial metals. Furthermore, it is able to produce ionized gas eclipses, which had previously been seen only for low-mass, non-degenerate companions in redback or black widow systems. We discuss the companion in relation to other sources, but find we understand neither its nature nor its origins. Thus, the system is interesting for understanding unusual stellar products of binary evolution, as well as, independent of its nature, for determining neutron-star masses.

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David L. Kaplan, Varun B. Bhalerao, Marten H. van Kerkwijk, Detlev Koester, Shri R. Kulkarni, Kevin Stovall. 2013-02-11. A Metal-Rich Low-Gravity Companion to a Massive Millisecond Pulsar. https://doi.org/10.1088/0004-637x%2F765%2F2%2F158

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