Volume 506, Number 3, November II 2009
|Page(s)||1269 - 1275|
|Section||Stellar structure and evolution|
|Published online||03 September 2009|
II. The V light curve
Instituto de Astrofísica de La Plata, CONICET, Paseo del bosque s/n, B1900FWA, La Plata, Argentina
2 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del bosque s/n, B1900FWA, La Plata, Argentina e-mail: firstname.lastname@example.org
3 Instituto de Ciencias Astronómicas de la Tierra y del Espacio, CONICET, Avda. España 1512 Sur, J5402DSP, San Juan, Argentina
4 Departamento de Física, Universidad de La Serena, Benavente 980, La Serena, Chile
Accepted: 1 August 2009
Context. WR 29 is a known WN7h+O double-lined binary system with a rather short period (3.164 days).
Aims. We search for light variations to determine the inclination of the system and thus the absolute masses of both components.
Methods. We observed photometrically the field of WR 29 between December, 2002, and February, 2006.
Results. We find that the V light of WR 29 varies in phase with the spectroscopic period of 3.16412 days, presenting two minima corresponding to the conjunctions of the binary components. Numerical models fitted to the light curve indicate an orbital inclination of about 44°, and masses of 53 and 42 for the O- and WN-type components, respectively.
Key words: stars: binaries: close / stars: binaries: eclipsing / stars: binaries: spectroscopic / stars: Wolf-Rayet
Full Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/1269
© ESO, 2009
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