EXOSAT guest observer program. Binary parameters of the X-ray Pulsar 4U1626-67

Details EXOSAT guest observer program. Binary parameters of the X-ray Pulsar 4U1626-67 EXOSAT guest observer program. Binary parameters of the X-ray Pulsar 4U1626-67

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987sao..reptr....m&link_type=abstract

Final Report, 1 Dec. 1986 - 30 Nov. 1987 Smithsonian Astrophysical Observatory, Cambridge, MA.

Other

Accretion Disks, Mass Transfer, Neutron Stars, Stellar Mass, X Ray Binaries, Companion Stars, Gravitational Waves, Stellar Evolution, Stellar Flares, Transfer Functions

Scientific paper

The pulsing X-ray source 4U1626-67 is an accreting neutron star in a binary system with a very low mass companion. The source was observed with EXOSAT continuously for 23 hr on 30 to 31 March 1986 UT. These observations allowed the setting of a stringent upper limit on the projected semimajor axis of the orbit of the neutron star of approx. 10 light msec for the 2485-s orbital period found by Middleditch et al., and a limit of approx. 13 light msec for any other plausible orbital period. The corresponding upper limit on the mass function for the 2485-s orbital period is 1.3 x 0.000001 solar mass. It was concluded that if the orbital inclination angle, i, equals 90 deg, then the optical companion star has a mass greater than 0.02 solar mass. However, it was found that a companion star mass greater than 0.06 solar mass is required if gravitational radiation is responsible for driving the mass transfer in this system. Only for i less than 16 deg can a companion star mass this large be accommodated by the limits set on the orbital amplitude. Also presented are results on the flaring activity in 4U1626-67 on time scales of approx. 1000 s, the energy dependent pulse profiles, and the pulse period history over the past decade.

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