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dc.contributor.authorTodt, Helge
dc.date.accessioned2010-10-12T18:22:37Z
dc.date.available2010-10-12T18:22:37Z
dc.date.issued2009
dc.identifier.urihttp://hdl.handle.net/11858/00-1735-0000-0001-308D-8
dc.description.abstractCentral 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.extent102 S.
dc.format.mimetypeapplication/pdf
dc.language.isoeng
dc.publisherUniv. Potsdam
dc.rights.urihttp://e-docs.geo-leo.de/rights
dc.subject.ddc523
dc.subject.gokTEG 000
dc.titleHydrogen-deficient central stars of planetary nebulae
dc.typemonograph
dc.subject.gokverbalKosmogonie {Astronomie}
dc.identifier.doi10.23689/FIDGEO-12
dc.identifier.ppn620379332
dc.identifier.urnurn:nbn:de:kobv:517-opus-41047
dc.type.versionpublishedVersion
dc.relation.collectionAstronomie, Astrophysik, Weltraumforschung
dc.description.typethesis


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