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AN M DWARF COMPANIO...
AN M DWARF COMPANION TO AN F-TYPE STAR IN A YOUNG MAIN-SEQUENCE BINARY
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- Eigmüller, Philipp (author)
- Deutsches Zentrums für Luft- und Raumfahrt (DLR),German Aerospace Center (DLR),Thüringer Landessternwarte Tautenburg
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- Eisloffel, J. (author)
- Thüringer Landessternwarte Tautenburg
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- Csizmadia, S. (author)
- Deutsches Zentrums für Luft- und Raumfahrt (DLR),German Aerospace Center (DLR)
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- Lehmann, H. (author)
- Thüringer Landessternwarte Tautenburg
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- Erikson, A. (author)
- Deutsches Zentrums für Luft- und Raumfahrt (DLR),German Aerospace Center (DLR)
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- Fridlund, Malcolm, 1952 (author)
- Chalmers tekniska högskola,Chalmers University of Technology
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- Hartmann, M. (author)
- Thüringer Landessternwarte Tautenburg
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- Hatzes, A. (author)
- Thüringer Landessternwarte Tautenburg
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- Pasternacki, T. (author)
- Deutsches Zentrums für Luft- und Raumfahrt (DLR),German Aerospace Center (DLR)
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- Rauer, H. (author)
- Deutsches Zentrums für Luft- und Raumfahrt (DLR),German Aerospace Center (DLR),Technische Universität Berlin
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- Tkachenko, A. (author)
- Katholieke Universiteit Leuven
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- Voss, H. (author)
- Universitat de Barcelona,University of Barcelona
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(creator_code:org_t)
- 2016-02-26
- 2016
- English.
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In: Astronomical Journal. - : American Astronomical Society. - 1538-3881 .- 0004-6256. ; 151:3
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Abstract
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- Only a few well characterized very low-mass M dwarfs are known today. Our understanding of M dwarfs is vital as these are the most common stars in our solar neighborhood. We aim to characterize the properties of a rare F+dM stellar system for a better understanding of the low-mass end of the Hertzsprung-Russel diagram. We used photometric light curves and radial velocity follow-up measurements to study the binary. Spectroscopic analysis was used in combination with isochrone fitting to characterize the primary star. The primary star is an early F-type main-sequence star with a mass of (1.493 +/- 0.073) M-circle dot and a radius of (1.474 +/- 0.040) R-circle dot. The companion is an M dwarf with a mass of (0.188 +/- 0.014) M-circle dot and a radius of (0.234 +/- 0.009) R-circle dot. The orbital period is (1.35121 +/- 0.00001) days. The secondary star is among the lowest-mass M dwarfs known to date. The binary has not reached a 1: 1 spin-orbit synchronization. This indicates a young main-sequence binary with an age below similar to 250 Myr. The mass-radius relation of both components are in agreement with this finding.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Keyword
- stars: evolution
- binaries: eclipsing
- stars: low-mass
- binaries: close
Publication and Content Type
- art (subject category)
- ref (subject category)
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- By the author/editor
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Eigmüller, Phili ...
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Eisloffel, J.
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Csizmadia, S.
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Lehmann, H.
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Erikson, A.
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Fridlund, Malcol ...
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show more...
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Hartmann, M.
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Hatzes, A.
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Pasternacki, T.
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Rauer, H.
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Tkachenko, A.
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Voss, H.
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- About the subject
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- NATURAL SCIENCES
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NATURAL SCIENCES
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and Physical Science ...
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and Astronomy Astrop ...
- Articles in the publication
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Astronomical Jou ...
- By the university
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Chalmers University of Technology