R Canis Majoris

R Canis Majoris is an eclipsing interacting binary star system in the constellation Canis Major. It varies from magnitude 5.7 to 6.34.[6] The system is unusual in the low ratio between the main two components and shortness of the orbital period.[3]

R Canis Majoris
Location of R CMa (circled)
Observation data
Epoch J2000.0      Equinox
Constellation Canis Major
Right ascension  07h 19m 28.18202s[1]
Declination −16° 23′ 42.8773″[1]
Apparent magnitude (V) 5.70 - 6.34[2]
Characteristics
Spectral type F0V + G8IV[3]
U−B color index +0.01[3]
B−V color index +0.34[3]
Variable type Algol
Astrometry
Radial velocity (Rv)-39.0[4] km/s
Proper motion (μ) RA: 165.37[1] mas/yr
Dec.: −136.18[1] mas/yr
Parallax (π)23.38 ± 0.54[1] mas
Distance44[3] pc
Absolute magnitude (MV)+2.57[5]
Details[3]
Mass1.67 + 0.22 + 0.8 M☉
Radius1.78 + 1.22 + 0.83 R☉
Luminosity8.2 + 0.49 + 0.4 L☉
Surface gravity (log g)4.16 + 3.60 + 4.50 cgs
Temperature6,964[5] K
Rotational velocity (v sin i)78.3±3.9[5] km/s
Other designations
R Canis Majoris, BD−16° 1898, HR 2788, HD 57167, HIP 35487, SAO 152724, GC 9758
Database references
SIMBADdata

Eclipse timings

Eclipse timings for R Canis Majoris have been being measured since 1887, and whilst at present the time period appears constant at 1.1359 days, periodic quasi-sinusoidal variations of the eclipse arrival times have been taking place with a periodicity of around 93 years. This has led to the suggestion that there exists a third non-eclipsing body in the system whose gravitational pull is responsible for these variations.[7]

Interacting binary star

R Canis Majoris is thought to be an interacting binary star. The secondary star has exceeded its Roche lobe and accreted mass to the primary star. This has resulted in the early evolution of the secondary star into the subgiant branch, and increased helium rich material in the primary, causing it to burn brighter and have a higher effective temperature than would usually be expected for a star of its mass.[8]

Reanalysis of the system using high-resolution spectroscopy yields its two main components to have masses 1.67 ± 0.08, and 0.22 ± 0.07 times that of the Sun respectively and radii 1.78 ± 0.03 and 1.22 ± 0.07 times that of the Sun respectively. Their surface temperatures are 7300 and 4350 K. The third star has a mass 80% that of the Sun and a radius around 83% that of the Sun. A third star in the system is very faint, presumably a red dwarf.[3]

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References
  1. Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. Budding, E.; Butland, R. (2011). "Observations and analysis of the system R Canis Majoris". Monthly Notices of the Royal Astronomical Society. 418 (3): 1764–73. Bibcode:2011MNRAS.418.1764B. doi:10.1111/j.1365-2966.2011.19597.x.
  4. Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  5. Ammler-von Eiff, M.; Reiners, A. (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724.
  6. Watson, Christopher (4 January 2010). "R Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 18 February 2014.
  7. “Astrometric and light-travel time orbits to detect low-mass companions: a case study of the eclipsing system R Canis Majoris” "Ribas I, Arenou F, & Guinan EF - The Astronomical Journal, 123:2033-2041, 2002 April
  8. ""Near-infrared photometric studies of R Canis Majoris" Varricatt WP & Ashok NM - The Astronomical Journal, 17:2980-2997, 1999 June". Retrieved 2009-03-08.
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