{"title":"软x射线瞬态和其他x射线双星中黑洞的动力学证据","authors":"A. Cowley","doi":"10.1063/1.45987","DOIUrl":null,"url":null,"abstract":"Although various observational properties have been suggested as indicators of a black hole in a binary system (e.g., rapid x‐ray fluctuations, ultra‐soft x‐ray spectra, etc.), the most certain way to determine the mass is to measure it dynamically, using observed radial velocities of the companion star. This paper discusses the x‐ray binaries for which such observational evidence for a stellar black hole is presently available.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"39 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Dynamical Evidence for Black Holes in Soft X-ray Transients and Other X-ray Binaries\",\"authors\":\"A. Cowley\",\"doi\":\"10.1063/1.45987\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"Although various observational properties have been suggested as indicators of a black hole in a binary system (e.g., rapid x‐ray fluctuations, ultra‐soft x‐ray spectra, etc.), the most certain way to determine the mass is to measure it dynamically, using observed radial velocities of the companion star. This paper discusses the x‐ray binaries for which such observational evidence for a stellar black hole is presently available.\",\"PeriodicalId\":101857,\"journal\":{\"name\":\"The evolution of X‐ray binaries\",\"volume\":\"39 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2008-05-12\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The evolution of X‐ray binaries\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1063/1.45987\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The evolution of X‐ray binaries","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.45987","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
Dynamical Evidence for Black Holes in Soft X-ray Transients and Other X-ray Binaries
Although various observational properties have been suggested as indicators of a black hole in a binary system (e.g., rapid x‐ray fluctuations, ultra‐soft x‐ray spectra, etc.), the most certain way to determine the mass is to measure it dynamically, using observed radial velocities of the companion star. This paper discusses the x‐ray binaries for which such observational evidence for a stellar black hole is presently available.
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