The orbital periods of aa dor and ny vir

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dc.contributor.authorKilkenny, Dave
dc.date.accessioned2023-03-01T13:03:31Z
dc.date.available2023-03-01T13:03:31Z
dc.date.issued2011
dc.description.abstractNew timings of eclipses made between 2000 and 2010 are presented for two binary systems with hot subdwarf primary stars. In the case of AA Dor, an sdOB star with a very cool secondary, the period is found to be constant at a level of about 10−14 d per orbit. In the case of NY Vir, a rapidly pulsating sdBVr with a cool companion, the period is discovered to be decreasing at a rate of −11.2 × 10−13 d per orbit. Close binary stars are particularly useful for the determination of fundamental stellar parameters. Double-lined spectroscopic binaries enable the mass ratio of the binary components to be determined and, if the inclination of the binary orbit can be measured or reasonably constrained (as in the case of an eclipsing system), then the absolute masses can be found. In addition, the light curve of an eclipsing system allows relative stellar radii to be found and even the absolute radii if the system is a double-lined binary.en_US
dc.identifier.citationKilkenny, D. (2011). The orbital periods of aa dor and ny vir. Monthly Notices of the Royal Astronomical Society, 412 (1) , 487-491. 10.1111/j.1365-2966.2010.17919.xen_US
dc.identifier.issn1365-2966
dc.identifier.uri10.1111/j.1365-2966.2010.17919.x
dc.identifier.urihttp://hdl.handle.net/10566/8486
dc.language.isoenen_US
dc.publisherOxford University Pressen_US
dc.subjectPhysicsen_US
dc.subjectAstronomyen_US
dc.subjectEclipsesen_US
dc.subjectBinary subdwarfen_US
dc.titleThe orbital periods of aa dor and ny viren_US
dc.typeArticleen_US

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