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Status: Bibliographieeintrag

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Verfasst von:Schweitzer, Andreas [VerfasserIn]   i
 Quirrenbach, Andreas [VerfasserIn]   i
 Kaminski, Adrian [VerfasserIn]   i
 Seifert, Walter [VerfasserIn]   i
Titel:The CARMENES search for exoplanets around M dwarfs
Titelzusatz:different roads to radii and masses of the target stars
Verf.angabe:A. Schweitzer, V.M. Passegger, C. Cifuentes, V.J.S. Béjar, M. Cortés-Contreras, J.A. Caballero, C. del Burgo, S. Czesla, M. Kürster, D. Montes, M.R. Zapatero Osorio, I. Ribas, A. Reiners, A. Quirrenbach, P.J. Amado, J. Aceituno, G. Anglada-Escudé, F.F. Bauer, S. Dreizler, S.V. Jeffers, E.W. Guenther, T. Henning, A. Kaminski, M. Lafarga, E. Marfil, J.C. Morales, J.H.M.M. Schmitt, W. Seifert, E. Solano, H.M. Tabernero, and M. Zechmeister
E-Jahr:2019
Jahr:14 May 2019
Umfang:16 S.
Fussnoten:Gesehen am 22.07.2019
Titel Quelle:Enthalten in: Astronomy and astrophysics
Ort Quelle:Les Ulis : EDP Sciences, 1969
Jahr Quelle:2019
Band/Heft Quelle:625(2019) Artikel-Nummer A68, 16 Seiten
ISSN Quelle:1432-0746
Abstract:Aims: We determine the radii and masses of 293 nearby, bright M dwarfs of the CARMENES survey. This is the first time that such a large and homogeneous high-resolution (R > 80 000) spectroscopic survey has been used to derive these fundamental stellar parameters. Methods: We derived the radii using Stefan-Boltzmann’s law. We obtained the required effective temperatures T-eff from a spectral analysis and we obtained the required luminosities L from integrated broadband photometry together with the Gaia DR2 parallaxes. The mass was then determined using a mass-radius relation that we derived from eclipsing binaries known in the literature. We compared this method with three other methods: (1) We calculated the mass from the radius and the surface gravity log g, which was obtained from the same spectral analysis as T-eff. (2) We used a widely used infrared mass-magnitude relation. (3) We used a Bayesian approach to infer stellar parameters from the comparison of the absolute magnitudes and colors of our targets with evolutionary models. Results: Between spectral types M0 V and M7 V our radii cover the range 0.1 R-circle dot < R < 0.6 R-circle dot with an error of 2-3% and our masses cover 0.09 M-circle dot < M < 0.6 M-cirle dot with an error of 3-5%. We find good agreement between the masses determined with these different methods for most of our targets. Only the masses of very young objects show discrepancies. This can be well explained with the assumptions that we used for our methods.
DOI:doi:10.1051/0004-6361/201834965
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext ; Verlag: https://doi.org/10.1051/0004-6361/201834965
 Volltext: https://www.aanda.org/articles/aa/abs/2019/05/aa34965-18/aa34965-18.html
 DOI: https://doi.org/10.1051/0004-6361/201834965
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1669581632
Verknüpfungen:→ Zeitschrift

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