Formation of the planet around the millisecond pulsar J1719–1438

Author： van Haaften L. M. Nelemans G. Voss R. Jonker P. G.

E-ISSN： 1432-0746|541|issue|A22-A22

ISSN： 0004-6361

Source： Astronomy & Astrophysics, Vol.541, Iss.issue, 2012-04, pp. : A22-A22

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Abstract

Context. Recently the discovery of PSR J1719–1438, a 5.8 ms pulsar with a companion in a 2.2 h orbit, was reported. The combination of this orbital period and the very low mass function is unique. The discoverers, Bailes et al. (2011, Science, 333, 1717), proposed an ultracompact X-ray binary (UCXB) as the progenitor system. However, the standard UCXB scenario would not produce this system as the time required to reach this orbital period exceeds the current estimate of the age of the Universe. The detached state of the system aggravates the problem. The inclination of the system is an important unknown, and Bailes et al. noted that for very low (a priori very unlikely) inclinations the system is better explained as having a brown dwarf companion rather than an UCXB origin.