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Precise orbit solution of MML 53, a low-mass, pre-main sequence eclipsing binary in Upper Centaurus Lupus
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
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2011 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 531, A61- p.Article in journal (Refereed) Published
Abstract [en]

Aims. We present a double-lined orbit solution for MML 53, the recently discovered low-mass pre-main sequence eclipsing binary. Methods. Using high-resolution spectra from the SMARTS 1.5 m echelle spectrograph, we measure precise radial velocities and derive the orbital parameters of the system. Results. The 2.1 d orbit of the eclipsing pair is circular, and we find the minimum masses of the eclipsing components to be M(1) sin(3) i = 0.97 M(circle dot) and M(2) sin(3) i = 0.84 M(circle dot), with formal uncertainties of 2.0% and an additional systematic uncertainty of approximate to 2.5% most likely caused by large star spots on the primary star. MML 53 has been previously identified as a member of the Upper Centaurus Lupus (UCL) star forming region (age similar to 15 Myr). The systemic radial velocity from our orbit solution, v(gamma) = + 1.4 +/- 0.3 +/- 0.8 km s(-1) (statistical and systematic), is also consistent with kinematic membership in this association. In addition, we detect a change in v(gamma) between 2006 and 2009 providing further evidence for the presence of a the third body in a wide (several year) orbit.

Place, publisher, year, edition, pages
2011. Vol. 531, A61- p.
Keyword [en]
binaries: eclipsing, stars: pre-main sequence, binaries: spectroscopic, stars: fundamental parameters, stars: individual: MML 53
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-158610DOI: 10.1051/0004-6361/201016249ISI: 000293017700056OAI: oai:DiVA.org:uu-158610DiVA: diva2:440115
Available from: 2011-09-12 Created: 2011-09-12 Last updated: 2012-10-11Bibliographically approved

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Stempels, Henricus Cornelis
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