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dc.contributor.authorVennes, Stéphane
dc.contributor.authorChayer, Pierre
dc.contributor.authorDupuis, Jean François
dc.contributor.authorLanz, Thierry M.
dc.date.accessioned2017-02-17T15:50:04Z
dc.date.available2017-02-17T15:50:04Z
dc.date.issued2006-12-01
dc.identifier.citationVennes, S., Chayer, P., Dupuis, J., & Lanz, T. (2006). Iron in hot DA white dwarfs. Astrophysical Journal, 652(2 I), 1554-1562. doi:10.1086/508509en_US
dc.identifier.urihttp://hdl.handle.net/11141/1168
dc.description.abstractWe present a study of the iron abundance pattern in hot, hydrogen-rich (DA) white dwarfs. The study is based on new and archival far-ultraviolet spectroscopy of a sample of white dwarfs in the temperature range 30,000 K ≲ Teff ≲ 64,000 K. The spectra obtained with the Far Ultraviolet Spectroscopic Explorer, along with spectra obtained with the Hubble Space Telescope Imaging Spectrograph and the International Ultraviolet Explorer, sample Fe III-Fe VI absorption lines, enabling a detailed iron abundance analysis over a wider range of effective temperatures than previously afforded. The measurements reveal abundance variations in excess of 2 orders of magnitude between the highest and the lowest temperatures probed, but also show considerable variations (over 1 order of magnitude) between objects with similar temperatures and surface gravities. Such variations in cooler objects may be imputed to accretion from unseen companions or so-called circumstellar debris, although the effect of residual mass loss and selective radiation pressure in the hottest objects in the sample remain dominant.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is made available in accordance with the publisher’s policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttps://aas.org/publications/aas-copyright-policyen_US
dc.titleIron in hot DA white dwarfsen_US
dc.typeArticleen_US
dc.identifier.doi10.1086/508509


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