Optical spectroscopy of the massive X-ray binary QV Nor (4U 1538 - 52)

Details Optical spectroscopy of the massive X-ray binary QV Nor (4U 1538 - 52) Optical spectroscopy of the massive X-ray binary QV Nor (4U 1538 - 52)

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256..631r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 4, June 15, 1992, p. 631-640. Research support

Astronomy and Astrophysics

Astronomy

33

Massive Stars, Optical Emission Spectroscopy, Stellar Mass, X Ray Binaries, Angular Velocity, H Alpha Line, Neutron Stars, Stellar Motions

Scientific paper

New spectroscopic mass estimates are obtained for both components of the massive wind-fed X-ray binary QV Nor. The mass of the primary star is found to be 19.9 +/- 3.4 solar masses, while the compact component has a most likely mass in the range 1.3 +/- 0.2 solar masses. The latter estimate places the neutron star in the expected 1.4 +/- 0.2 solar masses range, whereas the previous best estimate of 2 +/- 0.5 solar masses was the highest for any such object. The derived system parameters are shown to be consistent with the assumption of a fully filled Roche geometry, and the primary is not found to be significantly undermassive for its spectral class. No period change is reported. Studies of line profile variations are presented, based on measurements of the varying H-alpha feature and the 6678-A He I line. The H-alpha observations suggest the presence of an low-velocity outflow associated with the primary star, while the He I observations confirm the weakness of the incident X-ray flux on the stellar surface. No evidence for an accretion disk is found.

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