Masses of the components of SB2 binaries observed with Gaia. V. Accurate SB2 orbits for 10 binaries and masses of the components of 5 binaries

Double-lined spectroscopic binaries (SB2s) are one of the main sources of stellar masses, as additional observations are only needed to give the inclinations of the orbital planes in order to obtain the individual masses of the components. For this reason, we are observing a selection of SB2s using...

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Bibliographic Details
Published in:arXiv.org 2020-06
Main Authors: Halbwachs, Jean-Louis, Kiefer, Flavien, Lebreton, Yveline, Boffin, Henri M J, Arenou, Frédéric, Jean-Baptiste Le Bouquin, Famaey, Benoît, Pourbaix, Dimitri, Guillout, Patrick, Salomon, Jean-Baptiste, Mazeh, Tsevi
Format: Article
Language:English
Subjects:
Binary stars
Hertzsprung-Russell diagram
Interferometry
Orbital elements
Orbits
Radial velocity
Stellar evolution
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Summary:Double-lined spectroscopic binaries (SB2s) are one of the main sources of stellar masses, as additional observations are only needed to give the inclinations of the orbital planes in order to obtain the individual masses of the components. For this reason, we are observing a selection of SB2s using the SOPHIE spectrograph at the Haute-Provence observatory in order to precisely determine their orbital elements. Our objective is to finally obtain masses with an accuracy of the order of one percent by combining our radial velocity (RV) measurements and the astrometric measurements that will come from the Gaia satellite. We present here the RVs and the re-determined orbits of 10 SB2s. In order to verify the masses we will derive from Gaia, we obtained interferometric measurements of the ESO VLTI for one of these SB2s. Adding the interferometric or speckle measurements already published by us or by others for 4 other stars, we finally obtain the masses of the components of 5 binary stars, with masses ranging from 0.51 to 2.2 solar masses, including main-sequence dwarfs and some more evolved stars whose location in the HR diagram has been estimated.
ISSN:2331-8422
DOI:10.48550/arxiv.2006.01467