On the formation and evolution of black-hole binaries
We present the results of a systematic study of the formation and evolution of binaries containing black holes and normal-star companions with a wide range of masses. We first reexamine the standard formation scenario for close black-hole binaries, where the spiral-in of the companion in the envelop...
| Main Authors: | , , |
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| Format: | Journal article |
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2003
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| _version_ | 1826272298004381696 |
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| author | Podsiadlowski, P Rappaport, S Han, Z |
| author_facet | Podsiadlowski, P Rappaport, S Han, Z |
| author_sort | Podsiadlowski, P |
| collection | OXFORD |
| description | We present the results of a systematic study of the formation and evolution of binaries containing black holes and normal-star companions with a wide range of masses. We first reexamine the standard formation scenario for close black-hole binaries, where the spiral-in of the companion in the envelope of a massive star causes the ejection of the envelope. We estimate the formation rates for different companion masses and different assumptions about the common-envelope structure and other model parameters. We find that black-hole binaries with intermediate- and high-mass secondaries can form for a wide range of assumptions, while black-hole binaries with low-mass secondaries can only form with apparently unrealistic assumptions (in agreement with previous studies). We then present detailed binary evolution sequences for black-hole binaries with secondaries of 2 to 17 Msun and demonstrate that in these systems the black hole can accrete appreciably even if accretion is Eddington limited (up to 7 Msun for an initial black-hole mass of 10 Msun) and that the black holes can be spun up significantly in the process. We discuss the implications of these calculations for well-studied black-hole binaries (in particular GRS 1915+105), ultra-luminous X-ray sources and Cygnus X-1. Finally, we discuss how some of the assumptions in the standard model could be relaxed to allow the formation of low-mass, short-period black-hole binaries which appear to be very abundant in Nature. (Abstract abridged) |
| first_indexed | 2024-03-06T22:10:20Z |
| format | Journal article |
| id | oxford-uuid:5196d9b9-e7f5-4eba-8672-fc81b60946d8 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T22:10:20Z |
| publishDate | 2003 |
| record_format | dspace |
| spelling | oxford-uuid:5196d9b9-e7f5-4eba-8672-fc81b60946d82022-03-26T16:20:27ZOn the formation and evolution of black-hole binariesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:5196d9b9-e7f5-4eba-8672-fc81b60946d8Symplectic Elements at Oxford2003Podsiadlowski, PRappaport, SHan, ZWe present the results of a systematic study of the formation and evolution of binaries containing black holes and normal-star companions with a wide range of masses. We first reexamine the standard formation scenario for close black-hole binaries, where the spiral-in of the companion in the envelope of a massive star causes the ejection of the envelope. We estimate the formation rates for different companion masses and different assumptions about the common-envelope structure and other model parameters. We find that black-hole binaries with intermediate- and high-mass secondaries can form for a wide range of assumptions, while black-hole binaries with low-mass secondaries can only form with apparently unrealistic assumptions (in agreement with previous studies). We then present detailed binary evolution sequences for black-hole binaries with secondaries of 2 to 17 Msun and demonstrate that in these systems the black hole can accrete appreciably even if accretion is Eddington limited (up to 7 Msun for an initial black-hole mass of 10 Msun) and that the black holes can be spun up significantly in the process. We discuss the implications of these calculations for well-studied black-hole binaries (in particular GRS 1915+105), ultra-luminous X-ray sources and Cygnus X-1. Finally, we discuss how some of the assumptions in the standard model could be relaxed to allow the formation of low-mass, short-period black-hole binaries which appear to be very abundant in Nature. (Abstract abridged) |
| spellingShingle | Podsiadlowski, P Rappaport, S Han, Z On the formation and evolution of black-hole binaries |
| title | On the formation and evolution of black-hole binaries |
| title_full | On the formation and evolution of black-hole binaries |
| title_fullStr | On the formation and evolution of black-hole binaries |
| title_full_unstemmed | On the formation and evolution of black-hole binaries |
| title_short | On the formation and evolution of black-hole binaries |
| title_sort | on the formation and evolution of black hole binaries |
| work_keys_str_mv | AT podsiadlowskip ontheformationandevolutionofblackholebinaries AT rappaports ontheformationandevolutionofblackholebinaries AT hanz ontheformationandevolutionofblackholebinaries |