M. Huang

TL;DR: In this article, the authors reported the first subsolar chemical abundances of C and Si for U Geminorum with C down by 0.05 with respect to the Sun, almost certainly a result of C depletion due to thermonuclear processing.

TL;DR: In this paper, a reduced χ2 fit to the data reveals a DAZQ white dwarf with Teff = 22,500 ± 500 K, log g = 8, and photospheric abundances C = 0.5 solar, N = 5.0 solar, O = 2.2 solar, Si = 0., Fe = 0, and all other metals being 0.3 solar, with a rapidly spinning accretion belt with Vrot = 3350 km s-1, Tbelt = 26,000 ± 1000 K, and a fractional belt area

TL;DR: In this article, a pair of consecutive far-ultraviolet Goddard High-Resolution Spectrograph (GHRS) exposures of the Si IV region of the dwarf nova U Geminorum in early quiescence was obtained, 8 days after its return to optical quyingcence when the underlying white dwarf dominates the ultraviolet light of the system.

TL;DR: In this article, the authors presented the best-fitting synthetic spectra of the G140L spectra for the white dwarf in WZ Sge, exposed during quiescence, yielding a rapidly rotating white dwarf with velocity Vrot sin i = 1200+ 300−400 km s-1, white dwarf effective temperature Twd = 14,800 K, the gravity log g = 8.0, and the chemical abundances relative to solar in number (with 3σ error bars) of C, 5.0+ 2.0−2.

TL;DR: The first direct evidence of proton capture-processed material in the atmosphere of a white dwarf was found in the G160M spectra of the white dwarf in VW Hydri, exposed during quiescence as discussed by the authors.