Short-Period Light Variation of an Eclipsing Binary System: RZ Cassiopeiae

Ohshima, Osamu; Narusawa, S.; Akazawa, Hidehiko; Arai, K.; Fujii, M.; Kawabata, Tetsuya; Morikawa, Koichi; Ohkura, N.; Takeuti, M.

doi:10.1086/321109

Cited by 34 publications

(37 citation statements)

References 13 publications

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“…Since these differences of amplitudes, pulsation phases and frequency solutions could be resulted from spatial filtrations of non-radial modes during the primary eclipse (Mkrtichian et al 2002b), the hotter component of Y Cam should be excited in non-radial pulsation modes. In comparison with the case of Y Cam, pulsating components of AB Cas (Rodríguez et al 1998) and RZ Cas (Ohshima et al 2001) seem to be excited in radial modes, showing similar frequency solutions between the primary eclipsing phase data and the others. Further extensive photometric and spectroscopic observations during the primary eclipse of Y Cam would give us more detailed information on non-radial modes.…”

Section: Multiple Frequency Analysismentioning

confidence: 69%

“…Nevertheless, only six eclipsing binary stars were reported in a generalized review on δ Scuti stars in double and multiple systems by Lampens & Boffin (2000). So far, AB Cas (Rodríguez et al 1998) and RZ Cas (Ohshima et al 2001) have been studied photometrically in detail. This is probably due to difficulties in observing small amplitude oscillations, in comparison with large light variations caused by the eclipsing phenomenon.…”

Section: Introductionmentioning

confidence: 99%

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Photometric study of a pulsating component in the eclipsing binary Y Cam

Kim

Lee

Youn

et al. 2002

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Abstract. We present CCD photometric results of the eclipsing binary Y Cam, whose primary component has been known to be a δ Scuti type pulsator. Observations were performed for 16 nights, including two primary minima, from November 2000 to May 2001. After correction for light variations caused by the eclipsing phenomenon, we investigated its pulsating features in detail. We derived four pulsation frequencies of 15.0473 c/d, 18.2852 c/d, 14.8203 c/d and 17.7348 c/d using all data except for the primary eclipsing phase. The first frequency turned out to be constant over 40 years but the other frequencies have been changed or newly excited. It should be noted that V amplitude of the first frequency decreased to about a half in comparison with the previous results.

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Section: Multiple Frequency Analysismentioning

confidence: 69%

Section: Introductionmentioning

confidence: 99%

Photometric study of a pulsating component in the eclipsing binary Y Cam

Kim

Lee

Youn

et al. 2002

A&A

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“…There is only one known star that may be an Ap star and pulsates with periods in the range of Cunha's predicted periods: HD 13038 (Martinez et al 1999) with pulsation periods of 28 min and 34 min. Interestingly, there is also a δ Sct star (not a peculiar star) in an eclipsing binary system, RZ Cas, with a pulsation period of only 23 min (Ohshima et al 2001;Mkrtichian et al 2001). The pulsational behaviour of A stars in the δ Sct instability strip, or the roAp instability strip (if it really exists) in the period range of 15 min to 30 min is essentially unstudied observationally.…”

Section: Observations and Analysismentioning

confidence: 99%

A high-precision null result in the search for rapid oscillations in HD 965

Kurtz

Dolez

Chevreton

2003

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Abstract. HD 965 is a strongly magnetic peculiar A star with clear Zeeman splitting in its spectral lines, a rotation period greater than 2 yr, H-line core-wing anomaly, and strongly negative Strömgren δc 1 and δm 1 indices. All of these characteristics are typical of the rapidly oscillating Ap stars, and it has been suggested that HD 965 should be one. We have tested this star for photometric variability under excellent conditions with low scintillation noise using the 2-m TBL for 2.7 hr at Pic du Midi Observatory. The amplitude spectrum of the light curve is flat with noise peaks below 0.2 mmag in the frequency range of the roAp stars. This suggests that it is a non-oscillating Ap star, although proof of that will need further observations each year for many years, to rule out the possibility that rotational modulation has suppressed the observed amplitude in 2002.

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“…RZ Cas was found by Ohshima et al (1998Ohshima et al ( , 2001) to exhibit short-period light variability. They found a dominant oscillation mode of the primary with a frequency of 64.2 c d −1 and this frequency was later confirmed by means of dedicated Article published by EDP Sciences photometric campaigns by both Mkrtichian et al (2003) and Rodriguez et al (2004).…”

Section: Introductionmentioning

confidence: 96%

Spectroscopic modeling of oscillating Algol-type stars

Tkachenko

Lehmann

Mkrtichian

2009

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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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Short-Period Light Variation of an Eclipsing Binary System: RZ Cassiopeiae

Cited by 34 publications

References 13 publications

Photometric study of a pulsating component in the eclipsing binary Y Cam

Photometric study of a pulsating component in the eclipsing binary Y Cam

A high-precision null result in the search for rapid oscillations in HD 965

Spectroscopic modeling of oscillating Algol-type stars

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