Measuring the Boundary Layer and Inner Accretion Disk Temperatures for WX Ceti During Superoutburst

Abstract

We obtained EUV photometry, optical spectroscopy, and multi-color optical photometry for WX Cet during its 1998 November superoutburst. WX Cet is only the second short-period, low mass transfer CV (TOAD) to ever be observed in the EUV. Our determined superhump period is consistent with that found by Kato et al. (0.059 d) and we confirm that superhumps are grey in the optical. The optical spectra provide direct evidence that the line emission region is optically thick and our multi-wavelength photometric measurements are used to determine the inner accretion disk and boundary layer temperatures during superoutburst. Using a determined distance to WX Cet of ~130 pc, we find T${}_{ID}$= 21,000K and T_{BL}~72,500K. Both values are in good agreement with that expected by models of the superoutburst continuum being produced by the inner disk and boundary layer.

Accepted in PASP - July 2002 issue

References in corpus (2)

• HST Spectra of GW Librae: A Hot Pulsating White Dwarf in a Cataclysmic Variable
• 1998 Superoutburst of the Large-Amplitude SU UMa-Type Dwarf Nova WX Ceti

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• X-ray observations of historical classical nova counterparts with eROSITA telescope aboard SRG orbital observatory during the all-sky survey
• Photometry of Three Superoutbursts of the SU UMa-type Dwarf Nova, SW Ursae Majoris
• 2021 superoutburst of WZ Sge-type dwarf nova V627 Pegasi lacks an early superhump phase