On the nature of the binary radio pulsar PSR B0042-73 in the small magellanic cloud

Details On the nature of the binary radio pulsar PSR B0042-73 in the small magellanic cloud On the nature of the binary radio pulsar PSR B0042-73 in the small magellanic cloud

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...441..776l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 441, no. 2, p. 776-778

Computer Science

Numerical Analysis

5

Binary Stars, Black Holes (Astronomy), Magellanic Clouds, Pulsars, Stellar Evolution, Data Reduction, Numerical Analysis, Star Formation

Scientific paper

The modern scenario of evolution of massive binary systems predicts the existence of a subclass of binary radio pulsars (PSRs) with black holes (BHs). Their Galactic number was evaluated as approximately 1 per 1000 single pulsars (Lipunov et al. 1994b). Distinctive properties of such binaries would be (1) mass of the unseen companion Mc greater than 3-4 solar mass and (2) absence of eclipses of the pulsar radiation with no distinctive variance of the dispersion measure along the pulsar orbit. The pulsars themselves must be similar to standard isolated ones. The recently discovered binary 1 s pulsar PSR B0042-73 = PSR J0045-7319 in the Small Magellanic Cloud (SMC) with a massive companion in a highly elongated (eccentricity e =0.8) 51 day orbit (Kaspi et al. 1994) may be the first such pulsar with a BH. The paradoxical fact that the first pulsar discovered in the SMC proved to be in a binary system can be naturally understood if its companion actually is a 10-30 solar mass black hole. We illustrate this fact by the numerical calculation of evolution of radio pulsars after a star formation burst.

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