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High resolution spectroscopy of the triple system 20 Leo

Published online by Cambridge University Press:  12 April 2016

Y. Frémat ,
P. Lampens ,
H. Hensberge ,
T. Arentoft ,
P. De Cat ,
R. Garrido ,
L. Parrao ,
J.H. Peña ,
P. Mathias  and
P. Van Cauteren
Y. Frémat
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium
P. Lampens
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium
H. Hensberge
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium
T. Arentoft
Affiliation:
Department of Physics and Astronomy, Ny Munkegade, B. 520, Aarhus University, 8000 Aarhus C., Denmark
P. De Cat
Affiliation:
Instituut voor Sterrenkunde, Celestijnenlaan 200 B, 3001 Leuven, Belgium
R. Garrido
Affiliation:
Instituto de Astrofisica de Andalucia-CSIC, Apartado 3004, 18080 Granada, Spain
L. Parrao
Affiliation:
Instituto de Astronomia, Universidad Nacional Autonόma de México, Apartado 70-264, DF México
J.H. Peña
Affiliation:
Instituto de Astronomia, Universidad Nacional Autonόma de México, Apartado 70-264, DF México
P. Mathias
Affiliation:
Observatoire de la Côte d’Azur, BP 4229, 06304 Nice Cedex 4, France
P. Van Cauteren
Affiliation:
Beersel Hills Observatory, Laarkeidestraat 166, 1650 Beersel, Belgium

Abstract

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20 Leo is a spectroscopic triple system composed of 3 very similar stars, one of which seems to be a δ Sct star. Observations at high spectral and high time resolution have been obtained at the Observatoire de Haute Provence with the ELODIE spectrograph on the 1.9-m telescope. The spectra were taken during 7 nights in 2003 January and cover the whole optical domain from 3900 to 6800 Å. We used a Fourier transform technique recently developed by P. Hadrava to disentangle the combined spectrum. Application of the method allows the derivation of radial velocities at all orbital phases (even at phases of complete blending), as well as individual spectra for each component. From these computations we deduced more accurate individual radial velocities and improved orbital parameters describing the motion of the inner binary. Model atmospheres were used to analyze each individual spectrum and determine stellar fundamental parameters of the three components such as effective temperature, surface gravity and projected rotation velocity.

Type
Part 6. Binary stars and pulsation
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 395 - 398
Copyright
Copyright © Astronomical Society of the Pacific 2004

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