dc.contributor.author | Ferguson, D.H. | |
dc.contributor.author | Liebert, J. | |
dc.contributor.author | Haas, S. | |
dc.contributor.author | Napiwotzki, R. | |
dc.contributor.author | James, T.A. | |
dc.date.accessioned | 2007-12-17T09:58:00Z | |
dc.date.available | 2007-12-17T09:58:00Z | |
dc.date.issued | 1999 | |
dc.identifier.citation | Ferguson , D H , Liebert , J , Haas , S , Napiwotzki , R & James , T A 1999 , ' Masses and Other Parameters of the PostCommon Envelope Binary BE Ursae Majoris ' , The Astrophysical Journal , vol. 518 , pp. 866-872 . | |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | PURE: 168855 | |
dc.identifier.other | PURE UUID: 95b485f6-9c00-4812-90f2-3141a0d6a99a | |
dc.identifier.other | dspace: 2299/1230 | |
dc.identifier.other | Scopus: 0033587238 | |
dc.identifier.uri | http://hdl.handle.net/2299/1230 | |
dc.description | Original article can be found at: http://www.journals.uchicago.edu/ApJ/--Copyright American Astronomical Society | |
dc.description.abstract | The binary star BE Ursae Majoris is recently emerged from the common envelope phase; indeed, the hot sdO/DAO component is the central star of the associated planetary nebula. As such, BE UMa represents an important test case of stellar evolution theory. Using the Hubble Space Telescope (HST ) Goddard High Resolution Spectrograph (GHRS), we measured the radial velocity amplitude of the He II j1640 absorption line from the sdO/DAO component of this eclipsing system. Combining our results with those of Crampton, Cowley, & Hutchings, we determine stellar masses in units of solar mass as follows : for the sdO, the mass is 0.70^0.07, and that of the secondary star is 0.36^0.07, where we report the 1 p value for all errors. The separation between the component stars is 7.5 R and _^0.5 R_ is insensitive to small changes in inclination angle due to the near edge-on viewing angle of 84¡^1¡. Using these values, we modeled the eclipse light curve. Our results matched observed UBV R light curves of Wood and coworkers only if the modeled secondary star radius of 0.72 R has nearly _^0.05 R_ double the radius expected from the main-sequence mass-radius relation. The secondary star has thus not yet relaxed to thermal equilibrium since the common envelope phase ended D104 yr ago. Using the j1640 absorption-line proÐle and the surrounding continuum, we also were able to constrain the sdO helium abundance as log nHe\[1.1^0.2 and log nFe\1. Our results support the sdO/DAO log gD6.5 surface gravity and TeffD100,000 K values of Liebert et al. and are consistent with the post- AGB evolutionary track. Our best estimate of the distance to the BE UMa system is 2000 pc. | en |
dc.language.iso | eng | |
dc.relation.ispartof | The Astrophysical Journal | |
dc.title | Masses and Other Parameters of the PostCommon Envelope Binary BE Ursae Majoris | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | School of Physics, Engineering & Computer Science | |
dc.contributor.institution | Department of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research | |
dc.description.status | Peer reviewed | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |