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17th European White Dwarf Workshop: The white dwarf cooling age of NGC 6791
García-Berro, Enrique (2010)
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mla
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García-Berro E. "17th European White Dwarf Workshop: The white dwarf cooling age of NGC 6791.", timms video, Universität Tübingen (2010): https://timms.uni-tuebingen.de:443/tp/UT_20100817_004_eurowd_0001. Accessed 29 Oct 2020.
apa
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García-Berro, E. (2010). 17th European White Dwarf Workshop: The white dwarf cooling age of NGC 6791. timms video: Universität Tübingen. Retrieved October 29, 2020 from the World Wide Web https://timms.uni-tuebingen.de:443/tp/UT_20100817_004_eurowd_0001
harvard
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García-Berro, E. (2010). 17th European White Dwarf Workshop: The white dwarf cooling age of NGC 6791 [Online video]. 17 August. Available at: https://timms.uni-tuebingen.de:443/tp/UT_20100817_004_eurowd_0001 (Accessed: 29 October 2020).
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title: 17th European White Dwarf Workshop: The white dwarf cooling age of NGC 6791
alt. title: 17th European White Dwarf Workshop - White dwarf ages
creator: García-Berro, Enrique (author)
subjects: Astronomie, Physik, Astrophysik, Workshop, White Dwarf, cooling age, NGC 6791, Enrique García-Berro
description: 17th European White Dwarf Workshop, 16. bis 20. August 2010
abstract: The white dwarf cooling age of NGC 6791 (Enrique García-Berro1,2, Santiago Torres1,2, Leandro G. Althaus3, Isabel Renedo1,2, Pablo Lorén-Aguilar1,2, Alejandro H. Córsico3, René D. Rohrmann4, Maurizio Salaris5, Jordi Isern2,6) (1Universitat Politècnica de Catalunya, 2Institut d’Estudis Espacials de Catalunya, 3Universidad Nacional de La Plata, 4Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (CONICET), 5John Moores University, 6Institut de Ciències de l’Espai (CSIC)) NGC 6791 is a metal-rich ([Fe/H]=+0.4), well populated (~3,000 stars) and nearby (m - M = 13.44mag) open cluster that has been imaged down to luminosities below those of the faintest white dwarfs, allowing us to obtain a reliable white dwarf luminosity function. The main-sequence turn-off age (~8 Gyr) and the age derived from the termination of the white dwarf cooling sequence (~6 Gyr) are very different. One possible explanation is that as white dwarfs cool, one of the ashes of helium burning, 22Ne, sinks in the deep interior of these stars. At lower temperatures, white dwarfs are expected to crystallize and phase separation of 12C and 16O is expected to occur. This sequence of events is expected to introduce significant delays in the cooling times, but has not hitherto been proven. Here we present conclusive evidence that this indeed the case. We also assess the fraction of non-DA white dwarfs in the cluster, and we outline possible future applications of this cluster.
publisher: ZDV Universität Tübingen
contributor: ZDV Universität Tübingen (producer)
creation date: 2010-08-17
dc type: image
localtype: video
identifier: UT_20100817_004_eurowd_0001
language: eng
rights: Url: https://timmsstatic.uni-tuebingen.de/jtimms/TimmsDisclaimer.html?637395716799925325