SPECTROSCOPIC ANALYSIS OF THE R CANIS MAJORIS BINARY SYSTEM | Zendy

Napaporn A-thano | Zendy; D. E. Mkrtichian | Zendy; Siramas Komonjinda | Zendy

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SPECTROSCOPIC ANALYSIS OF THE R CANIS MAJORIS BINARY SYSTEM

Author(s) -

Napaporn A-thano,

D. E. Mkrtichian,

Siramas Komonjinda

Publication year - 2015

Publication title -

publications of the korean astronomical society

Language(s) - English

Resource type - Journals

eISSN - 2287-6936

pISSN - 1225-1534

DOI - 10.5303/pkas.2015.30.2.231

Subject(s) - physics , spectrograph , astrophysics , binary number , orbital period , primary (astronomy) , observatory , orbital elements , telescope , mass ratio , contact binary , binary star , orbital inclination , binary system , astronomy , spectral line , stars , mathematics , arithmetic

R Canis Majoris is a bright, short-period (1 d .1359) Algol-type eclipsing binary. For a long time, it was considered to be a low-mass binary star with M1 = 1.1M and M2 = 0.17M primary and secondary components, respectively (Tomkin, 1985). Glazunova, Yushchenko & Mkrtichian (2009) found new masses for the primary and secondary components of M1=1.81M and M2=0.23M , respectively and resolved a long-standing problem with the low masses of components for this binary. Budding and Butland (2011) conrmed the results of Glazunova, Yushchenko & Mkrtichian and obtained improved orbits and masses. New spectroscopic observations of R CMa were done during 8 nights on December 2012 with the 2.4-meter telescope of the Thai National Observatory (TNO) and bre-fed medium resolution echelle spectrograph. We obtained new, accurate orbital radial velocities of the two components of this binary system. Results of these investigations and the new orbital parameters are presented.

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