Radio and Optical Observations of the PSR:B1259-63 / SS:2883 Be-Star Binary System

Details Radio and Optical Observations of the PSR:B1259-63 / SS:2883 Be-Star Binary System Radio and Optical Observations of the PSR:B1259-63 / SS:2883 Be-Star Binary System

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.268..430j&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 268, NO. 2/MAY15, P. 430, 1994

Astronomy and Astrophysics

Astronomy

83

Inaries: Close - Stars: Emission-Line, Be - Stars: Individual: 55 2883 -- Pulsars: Individual: Psr B 1259-63 - Stars: Rotation - Radio Continuum: Stars

Scientific paper

We report here on radio timing observations of the 47-ms pulsar PSR B1259 -63 (PSR J1 302-6350) and optical observations of its binary companion Be star, 55 2883. The two are in a highly eccentric orbit of period 3.4 yr. Radio observations over 1250 days with the Parkes radio telescope now permit a phase-connected solution, which shows that' the next periastron is expected to occur on 1994 January 9.2 UT, and that the pulsar has a period derivative of 2.3 × 10-15. The pulsar thus has a characteristic age of 0.33 Myr and a surface magnetic field strength of 3 × 1011 G. Optical photometry of 55 2883 shows that the star is of spectral type of about B2e, indicating its mass to be 10 Msun and its radius 6 Rsun. The system can be no further than 1.5 kpc distant, substantially closer than the distance derived from the dispersion measure. High-resolution spectroscopy of the Balmer-series emission lines allows a determination of the underlying stellar rotation velocity, υ sin i, of 180 km s-1. It is likely that the inclination of the plane of the orbit and the inclination of the circumstellar disc are similar, at ˜35°. The system is a likely progenitor of the high-mass X-ray binaries and double-neutron-star systems such as PSR B1913+16.

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