The origin of sdB stars (II)
We have carried out a detailed binary populations synthesis (BPS) study of the formation of subdwarf B (sdB) stars and related objects (sdO, sdOB stars) using the latest version of the BPS code developed by Han et al.(1994, 1995a, 1995b, 1998, 2001). We systematically investigate the importance of t...
| Main Authors: | , , , |
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| Format: | Journal article |
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2003
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| _version_ | 1797054443857903616 |
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| author | Han, Z Podsiadlowski, P Maxted, P Marsh, T |
| author_facet | Han, Z Podsiadlowski, P Maxted, P Marsh, T |
| author_sort | Han, Z |
| collection | OXFORD |
| description | We have carried out a detailed binary populations synthesis (BPS) study of the formation of subdwarf B (sdB) stars and related objects (sdO, sdOB stars) using the latest version of the BPS code developed by Han et al.(1994, 1995a, 1995b, 1998, 2001). We systematically investigate the importance of the five main evolutionary channels in which the sdB stars form after one or two common-envelope (CE) phases, one or two phases of stable Roche-lobe overflow (RLOF) or as the result of the merger of two helium white dwarfs (WD) (see Han et al. 2002, Paper I). Our best BPS model can satisfactorily explain the main observational characteristics of sdB stars, in particular their distributions in the orbital period - minimum companion mass diagram and in the effective temperature - surface gravity diagram, their distributions of orbital period, log (g theta^4), and mass function, their binary fraction and the fraction of sdB binaries with WD companions, their birthrates and their space density. We obtain a Galactic formation rate, a total number in the Galaxy, the intrinsic binary fraction for sdB stars. We also predict a distribution of masses for sdB stars that is wider than is commonly assumed and that some sdB stars have companions of spectral type as early as B. The percentage of A type stars with sdB companions can in principle be used to constrain some of the important parameters in the binary evolution model. We conclude that (a) the first RLOF phase needs to be more stable than is commonly assumed; (b) mass transfer in the first stable RLOF phase is non-conservative, and the mass lost from the system takes away a specific angular momentum similar to that of the system; (c) common-envelope ejection is very efficient. |
| first_indexed | 2024-03-06T18:57:22Z |
| format | Journal article |
| id | oxford-uuid:124d7df2-a239-4e3a-806e-9c0f38e8a1e5 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T18:57:22Z |
| publishDate | 2003 |
| record_format | dspace |
| spelling | oxford-uuid:124d7df2-a239-4e3a-806e-9c0f38e8a1e52022-03-26T10:07:11ZThe origin of sdB stars (II)Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:124d7df2-a239-4e3a-806e-9c0f38e8a1e5Symplectic Elements at Oxford2003Han, ZPodsiadlowski, PMaxted, PMarsh, TWe have carried out a detailed binary populations synthesis (BPS) study of the formation of subdwarf B (sdB) stars and related objects (sdO, sdOB stars) using the latest version of the BPS code developed by Han et al.(1994, 1995a, 1995b, 1998, 2001). We systematically investigate the importance of the five main evolutionary channels in which the sdB stars form after one or two common-envelope (CE) phases, one or two phases of stable Roche-lobe overflow (RLOF) or as the result of the merger of two helium white dwarfs (WD) (see Han et al. 2002, Paper I). Our best BPS model can satisfactorily explain the main observational characteristics of sdB stars, in particular their distributions in the orbital period - minimum companion mass diagram and in the effective temperature - surface gravity diagram, their distributions of orbital period, log (g theta^4), and mass function, their binary fraction and the fraction of sdB binaries with WD companions, their birthrates and their space density. We obtain a Galactic formation rate, a total number in the Galaxy, the intrinsic binary fraction for sdB stars. We also predict a distribution of masses for sdB stars that is wider than is commonly assumed and that some sdB stars have companions of spectral type as early as B. The percentage of A type stars with sdB companions can in principle be used to constrain some of the important parameters in the binary evolution model. We conclude that (a) the first RLOF phase needs to be more stable than is commonly assumed; (b) mass transfer in the first stable RLOF phase is non-conservative, and the mass lost from the system takes away a specific angular momentum similar to that of the system; (c) common-envelope ejection is very efficient. |
| spellingShingle | Han, Z Podsiadlowski, P Maxted, P Marsh, T The origin of sdB stars (II) |
| title | The origin of sdB stars (II) |
| title_full | The origin of sdB stars (II) |
| title_fullStr | The origin of sdB stars (II) |
| title_full_unstemmed | The origin of sdB stars (II) |
| title_short | The origin of sdB stars (II) |
| title_sort | origin of sdb stars ii |
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