1H 1752 + 081: an eclipsing cataclysmic variable with a small accretion disk

Details 1H 1752 + 081: an eclipsing cataclysmic variable with a small accretion disk 1H 1752 + 081: an eclipsing cataclysmic variable with a small accretion disk

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...424..955s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 424, no. 2, p. 955-966

Astronomy and Astrophysics

Astronomy

27

Accretion Disks, Astronomical Models, Cataclysmic Variables, Eclipsing Binary Stars, H Beta Line, Visible Spectrum, White Dwarf Stars, X Ray Astronomy, X Ray Stars, Angular Momentum, Astronomical Catalogs, Astronomical Spectroscopy, Distance, Heao 1, Light Curve, Rosat Mission, Sky Surveys (Astronomy), Stellar Magnetic Fields, Stellar Mass

Scientific paper

We announce the discovery of an eclipsing nova-like cataclysmic variable (CV) as the optical counterpart to the HEAO 1 X-ray source 1H1752 + 081. This CV has an orbital period of 1.882801 hr, a high equivalent width of H-beta, and an average mv of 16.4 out of the eclipse. A geometric model is constructed from observations of the eclipse ingress and egress in many optical bandpasses. The broad-band emission originates primarily in two regions; the disk/accretion stream 'hot spot' and a compact central component, which may be a spot on the white dwarf surface, the entire white dwarf surface or the boundary layer between the accretion disk and the white dwarf surface. Based on the durations and offsets of the two eclipses we determined the mass ratio q = 2.5 +/- 0.6 and the angle of inclination i = 77 deg +/- 2 deg. If the central component is the entire white dwarf surface the masses of the stars are M1 = 0.80 +/- 0.06 solar masses and M2 = 0.32 +/- 0.06 solar masses. The disk is faint and small (RD = 0.25 +/- 0.05 rL1, where rL1 is the distance from the primary to the L1 point), compared to other eclipsing CVs. The small disk may result from the removal of angular momentum from the accretion disk by the magnetic field of the white dwarf; this CV may be a DQ Her type with a slowly rotating white dwarf. The emission-line velocities do not show the 'Z-wave' expected from the eclipse of a Keplerian accretion disk, nor do they have the correct phasing to originate near the white dwarf. The most likely origin of the line emission is the hot spot. The secondary star is visible at wavelengths greater than or equal to 6000 A during eclipse. We estimate a spectral type approximately M6 which, together with the observed m1 = 16.94 during eclipse, results in a distance estimate of 150 +/- 27 pc.

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