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17th European White Dwarf Workshop: Diffuse X-rays from PNe with WR-type central stars
Rühling, Ute (2010)
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mla
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Rühling U. "17th European White Dwarf Workshop: Diffuse X-rays from PNe with WR-type central stars.", timms video, Universität Tübingen (2010): https://timms.uni-tuebingen.de:443/tp/UT_20100817_016_eurowd_0001. Accessed 30 Oct 2020.
apa
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Rühling, U. (2010). 17th European White Dwarf Workshop: Diffuse X-rays from PNe with WR-type central stars. timms video: Universität Tübingen. Retrieved October 30, 2020 from the World Wide Web https://timms.uni-tuebingen.de:443/tp/UT_20100817_016_eurowd_0001
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Rühling, U. (2010). 17th European White Dwarf Workshop: Diffuse X-rays from PNe with WR-type central stars [Online video]. 17 August. Available at: https://timms.uni-tuebingen.de:443/tp/UT_20100817_016_eurowd_0001 (Accessed: 30 October 2020).
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title: 17th European White Dwarf Workshop: Diffuse X-rays from PNe with WR-type central stars
alt. title: 17th European White Dwarf Workshop - Central stars of planetary nebulae
creator: Rühling, Ute (author)
subjects: Astronomie, Physik, Astrophysik, Workshop, White Dwarf, diffuse X-rays, PNe, WR-type central stars, Ute Rühling
description: 17th European White Dwarf Workshop, 16. bis 20. August 2010
abstract: Diffuse X-rays from PNe with WR-type central stars (U. Rühling1,2, C. Sandin2, M. Steffen2, D. Schönberner2, W.-R. Hamann1, H. Todt1) (1Institut für Physik und Astronomie, Universität Potsdam, Germany, 2Astrophysikalisches Institut Potsdam, Germany) Planetary nebulae have been identified as weak, diffuse X-ray sources. Recently we added an observation of Abel 30 with XMM-Newton. We want to exploit the X-ray emission from PNe with hydrogen-deficient, [WC]-type central stars to constrain their still enigmatic origin. Different scenarios have been proposed, attributing the loss of hydrogen to a "late", "very late", or "AGB final" thermal pulse (LTP, VLTP, and AFTP, respectively). With a 1-D hydrodynamical code we model such nebulae, accounting for the stellar wind from the [WC]-type central star. For the first time, the models include a description of heat conduction in a hydrogen-poor plasma and we found that such heat conduction is able to cool the shocked gas sufficiently to achieve X-ray emitting temperatures. In case of a late thermal pulse, the fast central-star wind that sweeps up the nebula was hydrogen deficient from the beginning. Thus, the hot X-ray emitting bubble is expected to fill the whole nebula, showing a metal-rich, hydrogen-poor spectrum. A very late thermal pulse, on the other hand, occurs after a hydrogen-rich stellar wind already swept up the nebula. In this case, the X-ray emitting region is expected to be located closer to the central star. Although the X-ray observations suffer from the low brightness of the sources, we hope that the detailed comparison with the models will help to discriminate between different evolutionary scenarios.
publisher: ZDV Universität Tübingen
contributor: ZDV Universität Tübingen (producer)
creation date: 2010-08-17
dc type: image
localtype: video
identifier: UT_20100817_016_eurowd_0001
language: eng
rights: Url: https://timmsstatic.uni-tuebingen.de/jtimms/TimmsDisclaimer.html?637396140199020581