Near-Infrared Photometric Studies of RZ Cassiopeiae

Varricatt, W. P.; Ashok, N. M.; Chandrasekhar, T.

doi:10.1086/300517

Cited by 12 publications

(36 citation statements)

References 37 publications

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“…From the color indices, the effective temperature of the primary was derived by Rodriguez et al (2004) to be 8600 K, in agreement with Maxted et al (1994), whereas Varricatt et al (1998) adopted a higher temperature of 8720 K. The mass ratio is given as q = 0.331 by Maxted et al (1994). Soydugan et al (2006) analyzed both the light and radial velocity (RV hereinafter) curves based on photometric observations from 2002 and spectral data from 2003/2004 by using the Wilson-Devinney program (Wilson & Devinney 1971;van Hamme & Wilson 2003).…”

Section: Introductionsupporting

confidence: 52%

“…Theory predicts values of β = 0.08 for stars with convective envelopes (Lucy 1967), and β = 0.25 for those in hydrostatic and radiative equilibrium (von Zeipel 1924). In its original version, Shellspec07 applies a gravity darkening factor to the surface intensity that is assumed for the pole of the star.…”

Section: Gravity Darkeningmentioning

confidence: 99%

“…During primary minimum, a partial eclipse is observed . Olson (1982) and Varricatt et al (1998) found evidence of circumstellar matter surrounding the primary. Single-peaked emission originating from a structure located between the two stars was detected by Richards & Albright (1999).…”

Section: Introductionmentioning

confidence: 99%

“…Stellar and system parameters for RZ Cas were derived e.g., by Maxted et al (1994) from combined spectroscopy and UBV photometry (Chambliss 1976), by Varricatt et al (1998) from UBV (Chambliss 1976) and J and K band photometry, by Rodriguez et al (2004) from Stroemgren photometry, by Soydugan et al (2006) from combined spectroscopy and B and V band photometry, and by us (Papers I and II) from spectroscopy. From the color indices, the effective temperature of the primary was derived by Rodriguez et al (2004) to be 8600 K, in agreement with Maxted et al (1994), whereas Varricatt et al (1998) adopted a higher temperature of 8720 K. The mass ratio is given as q = 0.331 by Maxted et al (1994).…”

Section: Introductionmentioning

confidence: 99%

“…Varricatt et al (1998) mentioned that the best-fit model of the J band light curve is obtained by assuming a dark spot exists on the secondary.…”

Section: Introductionmentioning

confidence: 99%

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Spectroscopic modeling of oscillating Algol-type stars

Tkachenko

Lehmann

Mkrtichian

2009

A&A

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Aims. Based on time series of high-resolution spectra, we investigate the oEA star (i.e., Algol-type eclipsing binary with an oscillating primary component) RZ Cas to derive precise system and atmospheric parameters and search for phases of rapid mass-transfer and its effects on various system parameters at different epochs of observations. Methods. We combine a variety of methods including the KOREL program to decompose the components of the spectra and determine the orbital solution, the SynthV program to analyze the disentangled spectra by computing synthetic spectra based on atmosphere models, and the newly developed program Shellspec07_inverse to compute optimized stellar parameters from composite line profiles at all orbital phases. Results. Based on spectra taken in 2006, the RZ Cas system can be modeled accurately by assuming that only two stars are present. For spectra acquired in 2001, we obtained an improved solution by adding a light attenuating accretion annulus surrounding the primary, but were unable to model remaining structures in the O-C value distribution. The primary of RZ Cas is a normal A-type star that shows no λ Boo signatures, both components have close to solar abundance. The derived mass of the primary and the separation of the components are slightly smaller than previously assumed. The effective temperature of the primary of 8900 K, is 300 K higher than derived before. The Roche-lobe-filling secondary is assumed to have a large cool spot on its surface pointing towards the primary.

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Section: Introductionsupporting

confidence: 52%

Section: Gravity Darkeningmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…Varricatt et al (1998) mentioned that the best-fit model of the J band light curve is obtained by assuming a dark spot exists on the secondary.…”

Section: Introductionmentioning

confidence: 99%

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Spectroscopic modeling of oscillating Algol-type stars

Tkachenko

Lehmann

Mkrtichian

2009

A&A

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An Algol type binary with aδ Scuti component: RZ Cassiopeiae revisited

Soydugan

İbanoǧlu

et al. 2006

Astron. Nachr.

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We present new BV photometry and spectroscopic observations of RZ Cassiopeiae. The light and radial velocity curves were formed by the new observations which have been analyzed simultaneously by using the Wilson-Dewinney code. The non-synchronous rotational velocity v1 sin i = 76 ± 6 km s −1 , deduced for the primary component from the new spectroscopic observations, was also incorporated in the analysis. A time-series analysis of the residual light curves revealed the multi-periodic pulsations of the primary component of RZ Cas. The main peak in the frequency spectrum was observed at about 64.197 c d −1 in both B and V bands. The pulsational constant was calculated to be 0.0116 days. This value corresponds to high overtones (n ∼ 6) of non-radial mode oscillations. We find significant changes in the pulsational amplitude of the primary component from year to year. The peak-to-peak pulsational amplitude of the main frequency displays a decrease from 0.m 013 in 2000 to 0. m 002 in 2001 and thereafter we have found an increase again in the amplitude to 0. m 01 in the year 2002. We propose the mass transfer from the cool secondary to the pulsating primary as a possible explanation for such remarkable changes in the pulsational behavior of the primary component.

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Photometric Observations and Light Curve Studies of the Semi-Detached Eclipsing Binary R CMa

Mirtorabi¹,

Riazi

2006

Astrophys Space Sci

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We present observations and light curve analysis of the eclipsing binary R CMa in the narrow band filters v and b. Observations were made during 1993 at Biruni Observatory and the light curves have been analyzed using the Wilson-Devinney light curve interpretation program. Assuming a semi-detached configuration for R CMa, the parameters i, 1 , L 1 , T 2 and A 2 were adjusted for the best fit between the synthesized light curves and observations. Both light curves were fitted well with a lower value of bolometric albedo than what would be expected for a normal cool star with a convective envelope. The masses of the primary and secondary components and the absolute dimensions of the stars have been calculated using the derived relative dimensions from Wilson-Devinney codes and the spectroscopic observations.

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Near-Infrared Photometric Studies of RZ Cassiopeiae

Cited by 12 publications

References 37 publications

Spectroscopic modeling of oscillating Algol-type stars

Spectroscopic modeling of oscillating Algol-type stars

An Algol type binary with aδ Scuti component: RZ Cassiopeiae revisited

Photometric Observations and Light Curve Studies of the Semi-Detached Eclipsing Binary R CMa

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