Diese Anwendung erfordert Java-Skript.

Bitte aktivieren Sie Java-Script in den Browser-Einstellungen.
17th European White Dwarf Workshop: [WN] central stars of planetary nebulae
Todt, Helge (2010)
clipboard
mla
clipboard		 Todt H. "17th European White Dwarf Workshop: [WN] central stars of planetary nebulae.", timms video, Universität Tübingen (2010): https://timms.uni-tuebingen.de:443/tp/UT_20100817_015_eurowd_0001. Accessed 25 Apr 2024.
apa
clipboard		 Todt, H. (2010). 17th European White Dwarf Workshop: [WN] central stars of planetary nebulae. timms video: Universität Tübingen. Retrieved April 25, 2024 from the World Wide Web https://timms.uni-tuebingen.de:443/tp/UT_20100817_015_eurowd_0001
harvard
clipboard		 Todt, H. (2010). 17th European White Dwarf Workshop: [WN] central stars of planetary nebulae [Online video]. 17 August. Available at: https://timms.uni-tuebingen.de:443/tp/UT_20100817_015_eurowd_0001 (Accessed: 25 April 2024).
file download bibtex   endnote
Information
title: 17th European White Dwarf Workshop: [WN] central stars of planetary nebulae
alt. title: 17th European White Dwarf Workshop - Central stars of planetary nebulae
creator: Todt, Helge (author)
subjects: Astronomie, Physik, Astrophysik, Workshop, White Dwarf, [WN] central stars, planetary nebulae, Helge Todt
description: 17th European White Dwarf Workshop, 16. bis 20. August 2010
abstract: [WN] central stars of planetary nebulae (H. Todt1, M. Peña2, W.-R. Hamann1, G. Gräfener1,3) (1University of Potsdam, Institute for Physics and Astronomy, 14476 Potsdam, Germany, 2Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70264, México D.F. 04510, México, 3Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland) Hydrogen-deficient central stars are commonly considered as the progenitors of H-deficient white dwarfs. Spectroscopically, many H-deficient central stars resemble massive Wolf-Rayet stars of the carbon sequence and are therefore classified as [WC] stars. The massive WR stars of the nitrogen sequence (WN), however, have no spectroscopic counterpart among the central stars. By our analysis of PB 8 we found for the first time a central star with a WR-type emission line spectrum that belongs to the nitrogen sequence with only a slight enrichment of carbon, and therefore we classified this star as [WN/C]. Its chemical composition is very different from other Wolf-Rayet type central stars, containing mainly helium, some hydrogen, and only small amounts of carbon, nitrogen, and oxygen. In this context, we will also discuss the status of the central star of PMR 5, which is another candidate for a [WN] spectral type. The results of our analyses, especially the chemical composition, strongly constrains possible scenarios for the formation of PB 8. For the time being, we don’t know any path of single-star evolution that could explain this enigmatic central star.
publisher: ZDV Universität Tübingen
contributor: ZDV Universität Tübingen (producer)
creation date: 2010-08-17
dc type: image
localtype: video
identifier: UT_20100817_015_eurowd_0001
language: eng
rights: Url: https://timmsstatic.uni-tuebingen.de/jtimms/TimmsDisclaimer.html?638496431088830807