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17th European White Dwarf Workshop: The White Dwarf in SS Cygni - FUSE + HST Spectral Analysis
Sion, Edward (2010)
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mla
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Sion E. "17th European White Dwarf Workshop: The White Dwarf in SS Cygni - FUSE + HST Spectral Analysis.", timms video, Universität Tübingen (2010): https://timms.uni-tuebingen.de:443/tp/UT_20100819_001_eurowd_0001. Accessed 30 Oct 2020.
apa
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Sion, E. (2010). 17th European White Dwarf Workshop: The White Dwarf in SS Cygni - FUSE + HST Spectral Analysis. timms video: Universität Tübingen. Retrieved October 30, 2020 from the World Wide Web https://timms.uni-tuebingen.de:443/tp/UT_20100819_001_eurowd_0001
harvard
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Sion, E. (2010). 17th European White Dwarf Workshop: The White Dwarf in SS Cygni - FUSE + HST Spectral Analysis [Online video]. 19 August. Available at: https://timms.uni-tuebingen.de:443/tp/UT_20100819_001_eurowd_0001 (Accessed: 30 October 2020).
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title: 17th European White Dwarf Workshop: The White Dwarf in SS Cygni - FUSE + HST Spectral Analysis
alt. title: 17th European White Dwarf Workshop - White dwarfs in novae and CVs
creator: Sion, Edward (author)
subjects: Astronomie, Physik, Astrophysik, Workshop, White Dwarf, SS Cygni, FUSE, HST Spectral Analysis, Edward Sion
description: 17th European White Dwarf Workshop, 16. bis 20. August 2010
abstract: The White Dwarf in SS Cygni: FUSE + HST Spectral Analysis (E.M.Sion, P. Godon, J. Myzcka) (Villanova University) We have carried out a combined Hubble Space Telescope (HST/GHRS) and Far Ultraviolet Spectroscopic Explorer (FUSE) analysis of the prototype dwarf nova SS Cygni during quiescence. The FUSE and HST spectra were obtained at comparable times after outburst and have matching flux levels where the two spectra overlap. In our synthetic spectral analysis, we have used SS Cygni's accurate HST FGS parallax giving d = 166 pc, a newly determined mass for the accreting white dwarf (Bitner et al. 2007, ApJ) of Mwd = 0.81 M (Sun) (lower than the previous, widely used 1.2 M (Sun)) and the reddening (EB-V ) values 0.04 und 0.07 derived from the 2175 Å absorption feature in the IUE LWP spectra. From the best-fit model solutions to the combined HST + FUSE spectral energy distribution, we find that the white dwarf is reaching a temperature Teff approx. 45-55,000 K in quiescence, assuming log(g) = 8.3 with a solar composition accreted atmosphere. The exact temperature of the WD depends on the reddening assumed and on the inclusion of a quiescent low mass accretion rate accretion disk. Accretion disk models alone fit badly in the FUSE range while, and if we take the distance to be a free parameter, the only accretion disk model which fits well is for a discordant distance of at least several hundreds pc and an accretion rate (~ 10-8 M (Sun)/yr) which is unacceptably high for a dwarf nova in quiescence. We discuss the implications of the white dwarf's temperature on the time-averaged accretion rate and long term compressional heating models.
publisher: ZDV Universität Tübingen
contributor: ZDV Universität Tübingen (producer)
creation date: 2010-08-19
dc type: image
localtype: video
identifier: UT_20100819_001_eurowd_0001
language: eng
rights: Url: https://timmsstatic.uni-tuebingen.de/jtimms/TimmsDisclaimer.html?637396139987474238