The radius and mass of the subgiant star β Hyi from interferometry and asteroseismology
Identifieur interne : 000218 ( Main/Exploration ); précédent : 000217; suivant : 000219The radius and mass of the subgiant star β Hyi from interferometry and asteroseismology
Auteurs : J. R. North [Australie] ; J. Davis [Australie] ; T. R. Bedding [Australie] ; M. J. Ireland [Australie, États-Unis] ; A. P. Jacob [Australie] ; J. O'Byrne [Australie] ; S. M. Owens [Australie] ; J. G. Robertson [Australie] ; W. J. Tango [Australie] ; P. G. Tuthill [Australie]Source :
- Monthly Notices of the Royal Astronomical Society: Letters [ 1745-3925 ] ; 2007-09-01.
English descriptors
Abstract
We have used the Sydney University Stellar Interferometer to measure the angular diameter of β Hydri. This star is a nearby G2 subgiant the mean density of which was recently measured with high precision using asteroseismology. We determine the radius and effective temperature of the star to be 1.814 ± 0.017 R⊙ (0.9 per cent) and 5872 ± 44 K (0.7 per cent) respectively. By combining the radius with the mean density, as estimated from asteroseismology, we make a direct estimate of the stellar mass. We find a value of 1.07 ± 0.03 M⊙ (2.8 per cent), which agrees with published estimates based on fitting in the Hertzsprung–Russell diagram, but has much higher precision. These results place valuable constraints on theoretical models of β Hyi and its oscillation frequencies.
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DOI: 10.1111/j.1745-3933.2007.00355.x
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This star is a nearby G2 subgiant the mean density of which was recently measured with high precision using asteroseismology. We determine the radius and effective temperature of the star to be 1.814 ± 0.017 R⊙ (0.9 per cent) and 5872 ± 44 K (0.7 per cent) respectively. By combining the radius with the mean density, as estimated from asteroseismology, we make a direct estimate of the stellar mass. We find a value of 1.07 ± 0.03 M⊙ (2.8 per cent), which agrees with published estimates based on fitting in the Hertzsprung–Russell diagram, but has much higher precision. These results place valuable constraints on theoretical models of β Hyi and its oscillation frequencies.</div></front></TEI><affiliations><list><country><li>Australie</li><li>États-Unis</li></country></list><tree><country name="Australie"><noRegion><name sortKey="North, J R" sort="North, J R" uniqKey="North J" first="J. R." last="North">J. R. 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G." last="Tuthill">P. G. Tuthill</name></country><country name="États-Unis"><noRegion><name sortKey="Ireland, M J" sort="Ireland, M J" uniqKey="Ireland M" first="M. J." last="Ireland">M. J. Ireland</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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