HST Observations of WD1337+705: A New Determination of the Metal Accretion Rates

Details HST Observations of WD1337+705: A New Determination of the Metal Accretion Rates HST Observations of WD1337+705: A New Determination of the Metal Accretion Rates

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21925002d&link_type=abstract

American Astronomical Society, AAS Meeting #219, #250.02

Astronomy and Astrophysics

Astronomy

Scientific paper

WD1337+705 (EGGR 102, G 238-44)) is a DAZ white dwarf. Previous optical and UV observations have revealed high abundances of heavy elements in its atmosphere in spite of being in an effective temperature range where selective radiative acceleration of metals is not expected to be significant. Unlike many DAZ with high metal abundances, it does not exhibit a clear infrared excess that would normally indicate the presence of a dust disk around the star. In order to further our understanding of this star and related objects, we have acquired high resolution ultraviolet spectra of this star with the goal of characterizing the metallic content of its atmosphere through a detailed model atmosphere analysis of these spectra. Specifically, we focus on the analysis of the spectra recently obtained with the Cosmic Origin Spectrograph (COS) and STIS from which we report the detection of Al, Mg, and Fe. By combining these new measurements with time-dependent simulation of diffusion in presence of accretion, we put stringent constraints on the accretion rates for the different species detected and on the composition of the accreted matter.

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