The VLTI and its Subsystems

Glindemann, Andreas; Algomedo, J.; Amestica, Rodrigo; Ballester, P.; Bauvir, Bertrand; Bugueño, E.; Cabanero, S.; Correia, Serge; Delgado, Francisco; Delplancke, F.; Dérie, F.; Duhoux, Ph.; Folco, E. Di; Gennai, A.; Gilli, Bruno; Giordano, P.; Gitton, Ph.; Guisard, Stéphane; Housen, Nico; Huxley, Alexis; Kervella, P.; Kiekebusch, M.; Koehler, Bertrand; Lévêque, S.; Longinotti, Antonio; Ménardi, Serge; Morel, S.; Paresce, F.; Duc, Than Phan; Richichi, A.; Schöller, M.; Tarenghi, M.; Wallander, Anders; Wittkowski, M.; Wilhelm, Rainer

doi:10.1051/eas:2003008

Cited by 2 publications

(1 citation statement)

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“…For single stars we use observables such as magnitudes and colors (apart from oscillation frequencies) to estimate the mass. However, now that there are various possibilites of measuring a radius for single stars through interferometry (Paresce et al 2003;Glindemann et al 2003;Kervella et al 2003;Aufdenberg et al 2006) the question then arises: Can radius be used to determine the mass of the star?…”

Section: Introductionmentioning

confidence: 99%

The Complementary Roles of Interferometry and Asteroseismology in Determining the Mass of Solar‐Type Stars

Creevey

Monteiro

Metcalfe

et al. 2007

ApJ

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How important is an independent diameter measurement for the determination of stellar parameters of solar-type stars? When coupled with seismic observables, how well can we determine the stellar mass? If we can determine the radius of the star to between 1% and 4%, how does this affect the theoretical uncertainties? Interferometry can provide an independent radius determination and it has been suggested that we should expect at least a 4% precision on such a measurement for nearby solar-type stars. This study aims to provide both qualitative and quantitive answers to these questions for a star such as our Sun, where seismic information will be available. We show that the importance of an independent radius measurement depends on the combination of observables available and the size of the measurement errors. It is important for determining all stellar parameters and in particular the mass, where a good radius measurement can even allow us to determine the mass with a precision better than 2%. Our results also show that measuring the small frequency separation δν significantly improves the determination of the evolutionary stage τ and the mixing-length parameter α.

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Section: Introductionmentioning

confidence: 99%