CXOU J121538.2+361921 in the galaxy NGC 4214: a double neutron star in the making?
arXiv:astro-ph/0607068 · doi:10.1111/j.1745-3933.2006.00213.x
Abstract
CXOU J121538.2+361921 is the brightest X-ray source in the galaxy NGC 4214, with an X-ray luminosity of up to 0.7 x 10^39 erg/s. The observed periodicity of 3.62 hr is interpreted as the orbital period of the system. It has been suggested that the system is a low-mass helium star with a lower-mass compact companion. If this idea is correct, then CXOU J121538.2+361921 will evolve into a double neutron star, a binary consisting of a radio pulsar and another neutron star. In this study we investigate further this possibility. We find that the X-ray luminosity is consistent with super-Eddington accretion in a helium star-neutron star binary. The binary is in a state of mass transfer phase which is initiated when the helium-star donor is on the helium shell burning stage. A donor star with a current mass in the range of around 2.2 - 3.6 Msun is required to explain the observed orbital period. Helium stars in this mass range are massive enough to collapse in a supernova explosion, making CXOU J121538.2+361921 the immediate progenitor of a double neutron star.
arXiv commentMNRAS Lett., accepted
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