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Title:
Astrometric and Light-Travel Time Orbits to Detect Low-Mass Companions: A Case Study of the Eclipsing System R Canis Majoris
Authors:
Ribas, Ignasi; Arenou, Frédéric; Guinan, Edward F.
Affiliation:
AA(Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085; Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Avenida Diagonal 647, E-08028 Barcelona, Spain. ), AB(DASGAL, Observatoire de Paris, CNRS UMR 8633, F92195 Meudon Cedex, France ), AC(Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 )
Publication:
The Astronomical Journal, Volume 123, Issue 4, pp. 2033-2041. (AJ Homepage)
Publication Date:
04/2002
Origin:
UCP
Astronomy Keywords:
Astrometry, Stars: Binaries: Eclipsing, Stars: Fundamental Parameters, Stars: Individual: Constellation Name: R Canis Majoris, Stars: Late-Type
DOI:
10.1086/339560
Bibliographic Code:
2002AJ....123.2033R

Abstract

We discuss a method to determine orbital properties and masses of low-mass bodies orbiting eclipsing binaries. The analysis combines long-term eclipse timing modulations (the light-travel time [LTT] effect) with short-term, high-accuracy astrometry. As an illustration of the method, the results of a comprehensive study of Hipparcos astrometry and over 100 years of eclipse timings of the Algol-type eclipsing binary R Canis Majoris are presented. A simultaneous solution of the astrometry and the LTTs yields an orbital period of P12=92.8+/-1.3 yr, an LTT semiamplitude of 2574+/-57 s, an angular semimajor axis of a12=117+/-5 mas, and values of the orbital eccentricity and inclination of e12=0.49+/-0.05 and i12=91.7d+/-4.7d, respectively. Adopting the total mass of R CMa of M12=1.24+/-0.05 Msolar, the mass of the third body is M3=0.34+/-0.02 Msolar, and the semimajor axis of its orbit is a3=18.7+/-1.7 AU. From its mass, the third body is either a dM3-4 star or, more unlikely, a white dwarf. With the upcoming microarcsecond-level astrometric missions, the technique that we discuss can be successfully applied to detect and characterize long-period planetary-size objects and brown dwarfs around eclipsing binaries. Possibilities for extending the method to pulsating variables or stars with transiting planets are briefly addressed.
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