Diffusion in hot subdwarf progenitors from the common envelope channel
Diffusion of elements in the atmosphere of a star can drastically affect its surface composition, sometimes leading to unusual mixtures. These chemically peculiar stars can be identified fromthe presence of unusual lines in their spectra. Some hot subdwarf stars show extraordinary abundances of elem...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
| Published: |
De Gruyter
2017-12-01
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| Series: | Open Astronomy |
| Subjects: | |
| Online Access: | https://doi.org/10.1515/astro-2017-0440 |
| _version_ | 1818908021436186624 |
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| author | Byrne Conor M. Jeffery C. Simon Tout Christopher A. Hu Haili |
| author_facet | Byrne Conor M. Jeffery C. Simon Tout Christopher A. Hu Haili |
| author_sort | Byrne Conor M. |
| collection | DOAJ |
| description | Diffusion of elements in the atmosphere of a star can drastically affect its surface composition, sometimes leading to unusual mixtures. These chemically peculiar stars can be identified fromthe presence of unusual lines in their spectra. Some hot subdwarf stars show extraordinary abundances of elements such as lead, zirconium and strontium, while the abundance of helium ranges from practically zero to almost 100 percent across the hot subdwarf population. A sequence of extreme horizontal branch star models was generated by producing a number of post-common envelope objects from red giants. The evolution of these subdwarf progenitors was computed with the MESA stellar evolution code from immediately after envelope ejection right up to the ignition of helium in the core. Envelope abundances were calculated at the zero age horizontal branch for models both with and without the presence of diffusion. A small number of simulations also looked at the effects on radiative levitation of these abundances, to test how well diffusion physics is able to reproduce observational data. |
| first_indexed | 2024-12-19T22:04:23Z |
| format | Article |
| id | doaj.art-25c050587b104f58b2494d8dd1d4c8b5 |
| institution | Directory Open Access Journal |
| issn | 2543-6376 |
| language | English |
| last_indexed | 2024-12-19T22:04:23Z |
| publishDate | 2017-12-01 |
| publisher | De Gruyter |
| record_format | Article |
| series | Open Astronomy |
| spelling | doaj.art-25c050587b104f58b2494d8dd1d4c8b52022-12-21T20:04:04ZengDe GruyterOpen Astronomy2543-63762017-12-0126121421810.1515/astro-2017-0440astro-2017-0440Diffusion in hot subdwarf progenitors from the common envelope channelByrne Conor M.0Jeffery C. Simon1Tout Christopher A.2Hu Haili3Armagh Observatory & Planetarium, College Hill, Armagh, BT61 9DG, Northern IrelandArmagh Observatory & Planetarium, College Hill, Armagh, BT61 9DG, Northern IrelandInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKEarth Science Group, SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The NetherlandsDiffusion of elements in the atmosphere of a star can drastically affect its surface composition, sometimes leading to unusual mixtures. These chemically peculiar stars can be identified fromthe presence of unusual lines in their spectra. Some hot subdwarf stars show extraordinary abundances of elements such as lead, zirconium and strontium, while the abundance of helium ranges from practically zero to almost 100 percent across the hot subdwarf population. A sequence of extreme horizontal branch star models was generated by producing a number of post-common envelope objects from red giants. The evolution of these subdwarf progenitors was computed with the MESA stellar evolution code from immediately after envelope ejection right up to the ignition of helium in the core. Envelope abundances were calculated at the zero age horizontal branch for models both with and without the presence of diffusion. A small number of simulations also looked at the effects on radiative levitation of these abundances, to test how well diffusion physics is able to reproduce observational data.https://doi.org/10.1515/astro-2017-0440atomic processesstars: evolutionstars: subdwarfs |
| spellingShingle | Byrne Conor M. Jeffery C. Simon Tout Christopher A. Hu Haili Diffusion in hot subdwarf progenitors from the common envelope channel Open Astronomy atomic processes stars: evolution stars: subdwarfs |
| title | Diffusion in hot subdwarf progenitors from the common envelope channel |
| title_full | Diffusion in hot subdwarf progenitors from the common envelope channel |
| title_fullStr | Diffusion in hot subdwarf progenitors from the common envelope channel |
| title_full_unstemmed | Diffusion in hot subdwarf progenitors from the common envelope channel |
| title_short | Diffusion in hot subdwarf progenitors from the common envelope channel |
| title_sort | diffusion in hot subdwarf progenitors from the common envelope channel |
| topic | atomic processes stars: evolution stars: subdwarfs |
| url | https://doi.org/10.1515/astro-2017-0440 |
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