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On the evolution of o(he)-type stars
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Kruk, Jeffrey W. |
| Copyright Year | 2012 |
| Description | O(He) stars represent a small group of four very hot post-AGB stars whose atmospheres are composed of almost pure helium. Their evolution deviates from the hydrogen-deficient post-AGO evolutionary sequence of carbon-dominated stars like e.g. PG 1159 or Wolf- Rayet stars. While (very) late thermal pulse evolutionary models can explain the observed He/C/O abundances in these objects, they do not reproduce He-dominated surface abundances. Currently it seems most likely that the O(He) stars originate from a double helium white dwarf merger and so they could be the successors of the luminous helium-rich sdO-stars. An other possibility is that O(He)-stars could be successors of RCB or EHe stars. |
| File Size | 127741 |
| Page Count | 1 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_20120016010 |
| Archival Resource Key | ark:/13960/t74v1m228 |
| Language | English |
| Publisher Date | 2012-06-18 |
| Access Restriction | Open |
| Subject Keyword | Astrophysics Temperature Distribution Hot Stars Hydrogen Wolf-rayet Stars R Coronae Borealis Stars Stellar Evolution Asymptotic Giant Branch Stars Carbon Stars Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
