dc.contributor.author | Todt, Helge | |
dc.date.accessioned | 2010-10-12T18:22:37Z | |
dc.date.available | 2010-10-12T18:22:37Z | |
dc.date.issued | 2009 | |
dc.identifier.uri | http://hdl.handle.net/11858/00-1735-0000-0001-308D-8 | |
dc.description.abstract | Central stars of planetary nebulae are low-mass stars on the brink of their final evolution towards white dwarfs. Because of their surface temperature of above 25,000 K their UV radiation ionizes the surrounding material, which was ejected in an earlier phase of their evolution. Such fluorescent circumstellar gas is called a "Planetary Nebula". About one-tenth of the Galactic central stars are hydrogen-deficient. Generally, the surface of these central stars is a mixture of helium, carbon, and oxygen resulting from partial helium burning. Moreover, most of them have a strong stellar wind, similar to massive Pop-I Wolf-Rayet stars, and are in analogy classified as [WC]. The brackets distinguish the special type from the massive WC stars. | |
dc.format.extent | 102 S. | |
dc.format.mimetype | application/pdf | |
dc.language.iso | eng | |
dc.publisher | Univ. Potsdam | |
dc.rights.uri | http://e-docs.geo-leo.de/rights | |
dc.subject.ddc | 523 | |
dc.subject.gok | TEG 000 | |
dc.title | Hydrogen-deficient central stars of planetary nebulae | |
dc.type | monograph | |
dc.subject.gokverbal | Kosmogonie {Astronomie} | |
dc.identifier.doi | 10.23689/FIDGEO-12 | |
dc.identifier.ppn | 620379332 | |
dc.identifier.urn | urn:nbn:de:kobv:517-opus-41047 | |
dc.type.version | publishedVersion | |
dc.relation.collection | Astronomie, Astrophysik, Weltraumforschung | |
dc.description.type | thesis | |