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17th European White Dwarf Workshop: GD358 - The Case for Oblique Pulsation and Temperature Change
Montgomery, Michael (2010)
clipboard
mla
clipboard		 Montgomery M. "17th European White Dwarf Workshop: GD358 - The Case for Oblique Pulsation and Temperature Change.", timms video, Universität Tübingen (2010): https://timms.uni-tuebingen.de:443/tp/UT_20100820_010_eurowd_0001. Accessed 23 Apr 2024.
apa
clipboard		 Montgomery, M. (2010). 17th European White Dwarf Workshop: GD358 - The Case for Oblique Pulsation and Temperature Change. timms video: Universität Tübingen. Retrieved April 23, 2024 from the World Wide Web https://timms.uni-tuebingen.de:443/tp/UT_20100820_010_eurowd_0001
harvard
clipboard		 Montgomery, M. (2010). 17th European White Dwarf Workshop: GD358 - The Case for Oblique Pulsation and Temperature Change [Online video]. 20 August. Available at: https://timms.uni-tuebingen.de:443/tp/UT_20100820_010_eurowd_0001 (Accessed: 23 April 2024).
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Information
title: 17th European White Dwarf Workshop: GD358 - The Case for Oblique Pulsation and Temperature Change
alt. title: 17th European White Dwarf Workshop - Pulsating white dwarfs
creator: Montgomery, Michael (author)
subjects: Astronomie, Physik, Astrophysik, Workshop, White Dwarf, GD358, Oblique Pulsation, Temperature Change, Michael Montgomery
description: 17th European White Dwarf Workshop, 16. bis 20. August 2010
abstract: GD358: The Case for Oblique Pulsation and Temperature Change (M. H. Montgomery) (Department of Astronomy and McDonald Observatory, University of Texas at Austin, Austin, TX, USA) Convective driving, the mechanism originally proposed by Brickhill for pulsating white dwarf stars, has gained general acceptance as the generic linear instability mechanism in DAV and DBV white dwarfs. The nonlinear formulation of this mechanism is able to successfully reproduce the observed light curves of many pulsating white dwarfs, thereby providing information on the average depth of a pulsating white dwarf’s convection zone and the inclination angle of its pulsation axis. Using recent and archival data we provide a determination of the average depth of its convection zone in two different epochs, and we argue that the discrepancy between these determinations can be explained by a difference in surface temperature in the two epochs. In addition, we find that the oblique pulsation model provides an excellent fit to two sets of triplets found in the 2006 WET data. This marks the first time that oblique pulsation has been identified in a variable white dwarf star.
publisher: ZDV Universität Tübingen
contributor: ZDV Universität Tübingen (producer)
creation date: 2010-08-20
dc type: image
localtype: video
identifier: UT_20100820_010_eurowd_0001
language: eng
rights: Url: https://timmsstatic.uni-tuebingen.de/jtimms/TimmsDisclaimer.html?638495014181802698