R Canis Majoris---Revisited

Sarma, M. B. K.; Rao, P. Vivekananda; Abhyankar, K. D.

doi:10.1086/176820

Cited by 33 publications

(35 citation statements)

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“…Indeed, the present study is based on only one spectrum of the secondary and this is not completely satisfying. However, this spectrum was obtained using the 3.5 m NTT telescope at La Silla and we were extremely Sarma et al (1996) and Maxted & Hilditch (1996), and to this paper for TZ Eri (see Section 8.3). Primaries are identified with filled symbols and secondaries with open symbols.…”

Section: Resultsmentioning

confidence: 97%

“…8.3. Algol-type stars Sarma et al (1996) gave a detailed discussion on the evolutionary status of Algol components, on the basis of a comparison of their global parameters (masses, radii, luminosities, temperatures) with those of normal stars. As these authors noted :…”

Section: Distancementioning

confidence: 99%

“…9 and 10 present the Mass-Luminosity diagram (log L vs. log M ) and the HR diagram (log L vs. log T ) for the Algol systems in the lists by Sarma et al (1996) and Maxted & Hilditch (1996) having a mass of the primary smaller than 4 M ⊙ . The 3 systems with primaries off the main sequence (RZ Cnc, AR Mon, AW Peg) are not represented.…”

Section: Distancementioning

confidence: 99%

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Physical parameters of the Algol system VW Hydrae from simultaneous analysis of Geneva seven-colour light curves☆☆☆

2005

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Abstract. Light curves of the semi-detached eclipsing binary system TZ Eridani in the Geneva 7-colour photometric system were analysed using the Wilson-Devinney programme. The physical and orbital parameters have been determined through a self-consistent simultaneous solution of the seven light curves and of the radial velocity curves of both components. The following absolute elements of the components are, for the primary (mass gainer), M 1 = 1.97 ± 0.06 M ⊙ , R 1 = 1.69 ± 0.03 R ⊙ , M bol1 = 2.36 ± 0.09, T eff1 = 7770 ± 100 K, and for the secondary (mass loser), M 2 = 0.37 ± 0.01 M ⊙ , R 2 = 2.60 ± 0.04 R ⊙ , M bol2 = 3.74 ± 0.13, T eff2 = 4570 ± 100 K. The semi-major axis A of the relative orbit is 10.57 ± 0.16 R ⊙ . The regular increase of the period is described. The spectral type of the components are A5/6 V (primary) and K0/1 III. The secondary has exhibited a long-term luminosity increase of about 0.06 in V between Dec 1983 and Dec 1996. The distance to TZ Eri is evaluated to 270 ± 12 pc.

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Section: Resultsmentioning

confidence: 97%

Section: Distancementioning

confidence: 99%

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Physical parameters of the Algol system VW Hydrae from simultaneous analysis of Geneva seven-colour light curves☆☆☆

2005

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“…Several wellstudied systems of this kind are discussed in the literature. In particular, AS Eri (Popper 1980) and R CMa (Sarma et al 1996) are examples of Algols with parameters closely resembling those of V228. A comprehensive discussion of evolutionary models leading to the formation of such systems along with a summary of the observational data is given by Eggleton & KiselevaEggleton (2002) and Nelson & Eggleton (2001).…”

Section: Evolutionary Statusmentioning

confidence: 98%

The Clusters Ages Experiment (CASE). II. The Eclipsing Blue Straggler OGLEGC 228 in the Globular Cluster 47 Tuc

et al. 2007

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We use photometric and spectroscopic observations of the eclipsing binary OGLEGC 228 ( V228) to derive the masses, radii, and luminosities of the component stars. Based on measured systemic velocity, proper motion, and distance, the system is a blue straggler member of the globular cluster 47 Tuc. Our analysis shows that V228 is a semidetached Algol. We obtain M ¼ 1:512 AE 0:022 M , R ¼ 1:357 AE 0:019 R , and L ¼ 7:02 AE 0:050 L for the hotter and more luminous primary component and M ¼ 0:200 AE 0:007 M , R ¼ 1:238 AE 0:013 R , and L ¼ 1:57 AE 0:09 L for the Roche lobeYfilling secondary.

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“…Budding et al (1994) obtained B and V light curves of R CMa and derived the system parameters. Sarma, Rao, & Abhyankar (1996) analyzed the UBV and Ha light curves using a Wilson-Devinney model (Wilson & Devinney 1971). The luminosity of the primary and the secondary they derived were larger for masses of the corresponding components.…”

mentioning

confidence: 99%

Near-Infrared Photometric Studies of R Canis Majoris

Varricatt

Ashok

1999

The Astronomical Journal

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We present here the Ðrst light curves of the peculiar Algol binary system R Canis Majoris obtained in the near-infrared photometric bands J and K. The light curves are Ðtted for a semidetached model with the Wilson-Devinney light-curve synthesis program. The parameters of the system are derived. Published light curves in the optical photometric bands (U, B, V , and of Guinan, V light U n , B n , V n , Hb w , Hb n curve of Sato, and and light curves of Edalati, Khalesse, & Riazi) are reanalyzed and the Ha w Ha n results are compared. The temperature of the secondary component derived from the light-curve T 2 analysis shows an increase toward the near-IR wavelengths, achieving maximum in the K band. The secondary minima are deeper by 0.03 and 0.07 mag and the primary minima are shallower by 0.02 and 0.03 mag in the J and K bands, respectively, than what is expected in these bands from the secondary temperature and primary radius derived from the V band. In the case of the Ha and Hb light curves, the narrowband light curves yielded higher than the broadband light curves. The values of derived T 2 T 2 from these bands are found to be higher than those derived from the light curves observed in the neighboring wavelengths. We consider the possibility of the di †erence in the strength of photospheric absorption of Ha and Hb lines in the primary and the secondary as a reason for the high values of derived T 2 from these light curves.Five epochs of primary minima and four epochs of secondary minima are obtained in the present study. The increased depth of the secondary minima in the near-IR bands compared with the optical bands enabled us to determine the moments of secondary minima with nearly the same accuracy as those of primary minima. All the secondary minima appear at phase 0.5, and the durations are equal for the primary and the secondary eclipses. The epochs of primary minima follow the nearly sinusoidal O[C curve that has been observed for this star in previous studies. The values of O[C for the secondary minima were in the same range as those of the primary minima observed by us. We conclude that the system is in a circular orbit. Our observed epochs of primary minima support the presence of a third component in the system, as proposed by Radhakrishnan, Sarma, & Abhyankar. The e †ect of the presence of a third, noneclipsing, light source would be to suppress the observed depths of both the eclipses, whereas in this system we Ðnd that the secondary eclipse depth is being enhanced and the primary eclipse depth is being suppressed compared with expectations. So we have not Ðtted for a third light in our light-curve analysis, leaving the nature of the third body, if present, undetermined from our present light-curve analysis.The J-band light curve of R CMa Ðtted well with a bolometric albedo of the secondary star A 2 \ 0.5, as expected for a star with a convective atmosphere. But the K-band light curve showed a value of is also found to be higher in the broadband light curves than in the narrowband light A ...

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R Canis Majoris---Revisited

Cited by 33 publications

References 0 publications

Physical parameters of the Algol system VW Hydrae from simultaneous analysis of Geneva seven-colour light curves☆☆☆

Physical parameters of the Algol system VW Hydrae from simultaneous analysis of Geneva seven-colour light curves☆☆☆

The Clusters Ages Experiment (CASE). II. The Eclipsing Blue Straggler OGLEGC 228 in the Globular Cluster 47 Tuc

Near-Infrared Photometric Studies of R Canis Majoris

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