Properties of atmospheres and winds of H-deficient central stars and related objects
Abstract According to latest results presented at this workshop, it appears that thesurface chemistry of hydrogen-deficient post-AGB stars can now be explained byevolutionary calculations involving a late He-shell flash. A quantitativecomparison of theoretical predictions with observed element abund...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Werner, K. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2001 |
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| Schlagwörter: |
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| Anmerkung: |
© Kluwer Academic Publishers 2001 |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 275(2001), 1-2 vom: Jan., Seite 27-39 |
|---|---|
| Übergeordnetes Werk: |
volume:275 ; year:2001 ; number:1-2 ; month:01 ; pages:27-39 |
| Links: |
|---|
| DOI / URN: |
10.1023/A:1002735900499 |
|---|
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OLC2066225150 |
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| 520 | |a Abstract According to latest results presented at this workshop, it appears that thesurface chemistry of hydrogen-deficient post-AGB stars can now be explained byevolutionary calculations involving a late He-shell flash. A quantitativecomparison of theoretical predictions with observed element abundances caneventually constrain details of this evolutionary scenario. I will emphasizehere the diverse chemical compositions observed in H-deficient post-AGB stars,which call for an explanation. The abundance patterns vary from almost purehelium atmospheres to hydrogen- and helium-free atmospheres, with a richchoice of compositions in between, involving rather different mixtures of H,He, and CNO. | ||
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| 650 | 4 | |a Element Abundance | |
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10.1023/A:1002735900499 doi (DE-627)OLC2066225150 (DE-He213)A:1002735900499-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Werner, K. verfasserin aut Properties of atmospheres and winds of H-deficient central stars and related objects 2001 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2001 Abstract According to latest results presented at this workshop, it appears that thesurface chemistry of hydrogen-deficient post-AGB stars can now be explained byevolutionary calculations involving a late He-shell flash. A quantitativecomparison of theoretical predictions with observed element abundances caneventually constrain details of this evolutionary scenario. I will emphasizehere the diverse chemical compositions observed in H-deficient post-AGB stars,which call for an explanation. The abundance patterns vary from almost purehelium atmospheres to hydrogen- and helium-free atmospheres, with a richchoice of compositions in between, involving rather different mixtures of H,He, and CNO. Hydrogen Atmosphere Theoretical Prediction Late Result Element Abundance Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 275(2001), 1-2 vom: Jan., Seite 27-39 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:275 year:2001 number:1-2 month:01 pages:27-39 https://doi.org/10.1023/A:1002735900499 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 275 2001 1-2 01 27-39 |
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Abstract According to latest results presented at this workshop, it appears that thesurface chemistry of hydrogen-deficient post-AGB stars can now be explained byevolutionary calculations involving a late He-shell flash. A quantitativecomparison of theoretical predictions with observed element abundances caneventually constrain details of this evolutionary scenario. I will emphasizehere the diverse chemical compositions observed in H-deficient post-AGB stars,which call for an explanation. The abundance patterns vary from almost purehelium atmospheres to hydrogen- and helium-free atmospheres, with a richchoice of compositions in between, involving rather different mixtures of H,He, and CNO. © Kluwer Academic Publishers 2001 |
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Abstract According to latest results presented at this workshop, it appears that thesurface chemistry of hydrogen-deficient post-AGB stars can now be explained byevolutionary calculations involving a late He-shell flash. A quantitativecomparison of theoretical predictions with observed element abundances caneventually constrain details of this evolutionary scenario. I will emphasizehere the diverse chemical compositions observed in H-deficient post-AGB stars,which call for an explanation. The abundance patterns vary from almost purehelium atmospheres to hydrogen- and helium-free atmospheres, with a richchoice of compositions in between, involving rather different mixtures of H,He, and CNO. © Kluwer Academic Publishers 2001 |
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Abstract According to latest results presented at this workshop, it appears that thesurface chemistry of hydrogen-deficient post-AGB stars can now be explained byevolutionary calculations involving a late He-shell flash. A quantitativecomparison of theoretical predictions with observed element abundances caneventually constrain details of this evolutionary scenario. I will emphasizehere the diverse chemical compositions observed in H-deficient post-AGB stars,which call for an explanation. The abundance patterns vary from almost purehelium atmospheres to hydrogen- and helium-free atmospheres, with a richchoice of compositions in between, involving rather different mixtures of H,He, and CNO. © Kluwer Academic Publishers 2001 |
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| up_date |
2024-07-04T04:01:13.036Z |
| _version_ |
1803619583174639616 |
| fullrecord_marcxml |
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A quantitativecomparison of theoretical predictions with observed element abundances caneventually constrain details of this evolutionary scenario. I will emphasizehere the diverse chemical compositions observed in H-deficient post-AGB stars,which call for an explanation. 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7.399802 |