Observations and analysis of the system R Canis Majoris

Budding, E.; Butland, R.

doi:10.1111/j.1365-2966.2011.19597.x

Cited by 28 publications

(25 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Glazunova, Yushchenko & Mkrtichian (2009) found new masses for the primary and secondary components of M 1 =1.81M and M 2 =0.23M , respectively and resolved a long-standing problem with the low masses of components for this binary. Budding and Butland (2011) confirmed 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 fibre-fed medium resolution echelle spectrograph.…”

Section: Introductionsupporting

confidence: 88%

See 1 more Smart Citation

Spectroscopic Analysis of the R Canis Majoris Binary System

A-thano¹,

Mkrtichian²,

Komonjinda³

2015

Publications of The Korean Astronomical Society

View full text Add to dashboard Cite

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 M 1 = 1.1M and M 2 = 0.17M primary and secondary components, respectively (Tomkin, 1985). Glazunova, Yushchenko & Mkrtichian (2009) found new masses for the primary and secondary components of M 1 =1.81M and M 2 =0.23M , respectively and resolved a long-standing problem with the low masses of components for this binary. Budding and Butland (2011) confirmed 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 fibre-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.

show abstract

Section: Introductionsupporting

confidence: 88%

“…They found new accurate masses of the primary and secondary components of M 1 =1.81 M and M 2 =0.23 M , respectively. Recent high-resolution spectroscopic investigation of R CMa by Budding & Butland (2011) confirmed the masses of components found by http://pkas.kas.org Glazunova et al(2009). Their improved accurate parameters are:…”

Section: Introductionsupporting

confidence: 62%

Spectroscopic Analysis of the R Canis Majoris Binary System

A-thano¹,

Mkrtichian²,

Komonjinda³

2015

Publications of The Korean Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The unusual combination of short period and low mass ratio in this group may also be related to angular momentum redistribution in the presence of third bodies as suspected by e.g. Budding & Butland (2011). This could be relevant to the present case, where orbital angular momentum may well have been redistributed in this old Algol, while tidal coupling, given the low mass of the secondary, may have been insufficient to spin up the primary.…”

Section: Discussionmentioning

confidence: 54%

“…A reasonable fit to the data could only be obtained by assuming a higher albedo for the primary than physically expected and an unusually low mass ratio of q = 0.0626. Together with the short period, these properties would make KIC 10661783 a member of the subgroup of R CMa stars among the Algol-type stars (see Varricatt & Ashok 1999 for a discussion; Budding & Butland 2011 for R CMa). The mass ratio is a critical piece of information when assessing wether the secondary component fills its critical Roche lobe (RL) or not, i.e.…”

Section: Introductionmentioning

confidence: 99%

Physical properties of the eclipsingδ Scuti star KIC 10661783

Lehmann

Southworth

Tkachenko

et al. 2013

A&A

View full text Add to dashboard Cite

Context. KIC 10661783 is an eclipsing binary that shows δ Scuti-like oscillations. More than 60 pulsation frequencies have been detected in its light curve as observed by the Kepler satellite. Aims. We want to determine the fundamental stellar and system parameters of the eclipsing binary as a precondition for asteroseismic modelling of the pulsating component and to establish whether the star is a semi-detached Algol-type system. Methods. We measured the radial velocities of both components from new high-resolution spectra using TODCOR and compute the orbit using PHOEBE. We used the KOREL program to decompose the observed spectra into its components, and analysed the decomposed spectra to determine the atmospheric parameters. For this, we developed a new computer program for the normalisation of the KOREL output spectra. Fundamental stellar parameters are determined by combining the spectroscopic results with those from the analysis of the Kepler light curve. Results. We obtain T eff , log g, v sin i, and the absolute masses and radii of the components, together with their flux ratio and separation. Whereas the secondary star rotates synchronously with the orbital motion, the primary star rotates subsynchronously by a factor of 0.75. The newly determined mass ratio of 0.0911 is higher than previously thought and means a detached configuration is required to fit the light curve. Conclusions. With its low orbital period and very low mass ratio, the system shows characteristics of the R CMa-type stars but differs from this group by being detached. Its current state is assumed to be that of a detached post-Algol binary system with a pulsating primary component.

show abstract

“…The primary and secondary components fill F 1 = 45 % and F 2 = 99 % of their limiting lobe, respectively, where the filling factor F 1,2 = Ω in /Ω 1,2 . With its small q and short P , our program target closely resembles the two Kepler pulsating EBs KIC 10661783 (Lehmann et al 2013) and KIC 8262223 (Guo et al 2016), which are detached binaries with characteristics of the R CMa-type stars (Budding & Butland 2011;Lee et al 2016b) among Algols. A comparison of the KIC 11401845 parameters with the mass-radius, mass-luminosity, and Hertzsprung-Russell (HR) diagrams (Ibanoǧlu et al 2006) shows that the primary component resides within the mainsequence band.…”

Section: Discussionmentioning

confidence: 99%

KIC 11401845: An Eclipsing Binary with Multiperiodic Pulsations and Light-travel Time

Lee

Hong

Koo

2017

ApJ

View full text Add to dashboard Cite

We report the Kepler photometry of KIC 11401845 displaying multiperiodic pulsations, superimposed on binary effects. Light-curve synthesis represents that the binary star is a short-period detached system with a very low mass ratio of q = 0.070 and filling factors of F 1 = 45 % and F 2 = 99 %. Multiple frequency analyses were applied to the light residuals after subtracting the synthetic eclipsing curve from the observed data. We detected 23 frequencies with signal to noise amplitude ratios larger than 4.0, of which the orbital harmonics (f 4 , f 6 , f 9 , f 15 ) in the low frequency domain may originate from tidally excited modes. For the high frequencies of 13.7−23.8 day −1 , the period ratios and pulsation constants are in the ranges of P pul /P orb = 0.020−0.034 and Q = 0.018−0.031 d, respectively. These values and the position on the Hertzsprung-Russell diagram demonstrate that the primary component is a δ Sct pulsating star. We examined the eclipse timing variation of KIC 11401845 from the pulsation-subtracted data and found a delay of 56±17 s in the arrival times of the secondary eclipses relative to the primary eclipses. A possible explanation of the time shift may be some combination of a light-travel-time delay of about 34 s and a very small eccentricity of e cos ω < 0.0002. This result represents the first measurement of the Rømer delay in non-compact binaries.

show abstract

Observations and analysis of the system R Canis Majoris

Cited by 28 publications

References 37 publications

Spectroscopic Analysis of the R Canis Majoris Binary System

Spectroscopic Analysis of the R Canis Majoris Binary System

Physical properties of the eclipsingδ Scuti star KIC 10661783

KIC 11401845: An Eclipsing Binary with Multiperiodic Pulsations and Light-travel Time

Contact Info

Product

Resources

About