A spectroscopic, photometric, and X-ray study of the DQ Herculis system 1H0542-407

Details A spectroscopic, photometric, and X-ray study of the DQ Herculis system 1H0542-407 A spectroscopic, photometric, and X-ray study of the DQ Herculis system 1H0542-407

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...344..376b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 344, Sept. 1, 1989, p. 376-398.

Astronomy and Astrophysics

Astronomy

60

Astronomical Photometry, Astronomical Spectroscopy, Dwarf Novae, Magnetic Stars, X Ray Astronomy, X Ray Binaries, Balmer Series, M Stars, Stellar Models, Stellar Orbits, Stellar Rotation, White Dwarf Stars

Scientific paper

Spectroscopic and photometric observations of the DQ Herculis binary 1H0542-407 are reported, and models are derived based on these and earlier observations. The system consists of a high-mass, about 1.3 solar mass white dwarf with a spin period of 1911 sec in a 5.7-h orbital period with about a 0.6 solar mass M0 dwarf secondary. The system is viewed at low inclination, so that only one accreting pole is observed. An accretion disk is disrupted by the white dwarf's magnetic field at a distance of about 20,000 km. The gas subsequently accretes along the field lines in the manner of an auroral curtain or arc. A strong shock is produced just above the surface, with the hot gas cooling via bremsstrahlung emission, producing a luminosity of (5-10) x 10 to the 34th ergs/sec. It is shown that the magnetospheric gating model is inapplicable to the star unless the magnetic field strength is inordinately high.

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