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17th European White Dwarf Workshop: On the formation of Main Sequence-massive WD binaries
Ferrario, Lilia (2010)
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mla
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Ferrario L. "17th European White Dwarf Workshop: On the formation of Main Sequence-massive WD binaries.", timms video, Universität Tübingen (2010): https://timms.uni-tuebingen.de:443/tp/UT_20100819_009_eurowd_0001. Accessed 30 Oct 2020.
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Ferrario, L. (2010). 17th European White Dwarf Workshop: On the formation of Main Sequence-massive WD binaries. timms video: Universität Tübingen. Retrieved October 30, 2020 from the World Wide Web https://timms.uni-tuebingen.de:443/tp/UT_20100819_009_eurowd_0001
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Ferrario, L. (2010). 17th European White Dwarf Workshop: On the formation of Main Sequence-massive WD binaries [Online video]. 19 August. Available at: https://timms.uni-tuebingen.de:443/tp/UT_20100819_009_eurowd_0001 (Accessed: 30 October 2020).
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title: 17th European White Dwarf Workshop: On the formation of Main Sequence-massive WD binaries
alt. title: 17th European White Dwarf Workshop - White dwarfs in detached binaries
creator: Ferrario, Lilia (author)
subjects: Astronomie, Physik, Astrophysik, Workshop, White Dwarf, Main Sequence-massive WD binaries, formation, Lilia Ferrario
description: 17th European White Dwarf Workshop, 16. bis 20. August 2010
abstract: On the formation of Main Sequence-massive WD binaries (Lilia Ferrario and Dayal Wickramasinghe) (Mathematical Sciences Institute, The Australian National University, Canberra) Although some 20 - 30% of all white dwarfs are found paired wih M-dwarfs, there are no known high field magnetic white dwarfs with a detached M-dwarf companion. Such pairings also seem to be uncommon in the general class of massive white dwarfs in detached binaries, regardless of whether they are strongly magnetic or not. Taking note of the fact that high field magnetic white dwarfs tend to have high-mass progenitors, we propose that the above result may be a direct consequence of the manner in which stars with primary masses M1 are paired with secondary masses M2 equqal or less than M1 on the main sequence. Our calculations suggest that primaries with masses greater than about 3 solar masses that evolve into the more massive white dwarfs tend to pair with M-dwarf secondaries in a region of the mass ratio distribution f(q) (q = M2/M1 equal or less than 1) that decreases with decrease in q. On the other hand, the less massive primaries that evolve into the bulk of observed white dwarfs have companions in a region of the f(q) distribution that is consistent with these being distributed according to an Initial Mass Function peaking near M = 0.2 - 0.3, such as that derived by Chabrier (2005).
publisher: ZDV Universität Tübingen
contributor: ZDV Universität Tübingen (producer)
creation date: 2010-08-19
dc type: image
localtype: video
identifier: UT_20100819_009_eurowd_0001
language: eng
rights: Url: https://timmsstatic.uni-tuebingen.de/jtimms/TimmsDisclaimer.html?637396138113060599