On the nature of the binary radio pulsar PSR B0042-73 in the SMC

Details On the nature of the binary radio pulsar PSR B0042-73 in the SMC On the nature of the binary radio pulsar PSR B0042-73 in the SMC

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994astl...20..588l&link_type=abstract

Astronomy Letters, Volume 20, Issue 5, September 1994, pp.588-590; Pis'ma v Astronomicheskii Zhurnal, Vol. 20, p. 684

Astronomy and Astrophysics

Astronomy

Scientific paper

The modem scenario of the evolution of massive binary systems predicts the existence of binary radio pulsars (PSR) with black holes (BH) that are sufficiently numerous [1] to be discovered in the near future. Distinctive properties of such binaries are the mass of an unseen companion M_c_ > 3 - 4 M_sun_, the absence of eclipses of the radio pulsar, and no noticeable variations of the dispersion measure during the pulsar orbital motion. Proper parameters of the radio pulsar with a black hole must not differ from the parameters of a standard isolated pulsar. The recently discovered first radio pulsar in the Small Magellanic Cloud (SMC) PSR B0002-73 = PSR J0044-73 [2] is a member of a binary system with a massive companion in an eccentric orbit (e = 0.8) with a period of 51 days, and may turn out to be the first radio pulsar with a BH. The paradoxical fact that the first pulsar discovered in the SMC proved to be binary appears to be quite natural if its companion is a 10 - 30 M_sun_ black hole. This fact is illustrated by a numerical calculation of evolution of radio pulsars born in a star-formation burst.

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