The eclipsing binary star RZ Cassiopeiae

Lehmann, H.; Mkrtichian, D. E.

doi:10.1051/0004-6361:20078865

Cited by 16 publications

(12 citation statements)

References 19 publications

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“…Note that at least for three systems, namely RW Mon (Mukherjee et al 1996), RZ Cas (Lehmann & Mkrtichian 2008), and TW Dra (Van Hamme & Wilson 1990), the values of asynchronicity were decreased from F = 1.3-1.4 to F = 1.0 as a result of new, accurate determinations of the radii of the components and of the rotational velocities.…”

Section: Introductionmentioning

confidence: 92%

Rotational Velocities of the Components of 23 Binaries

Glazunova

Yushchenko

Tsymbal

et al. 2008

The Astronomical Journal

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By using high dispersion spectra obtained by the 1.8 m telescope of Bohyunsan Optical Astronomy Observatory (South Korea), multiline least-square deconvolution of line profiles, and Fourier analysis techniques, we obtained the rotational velocities of the components of 23 binary systems. The rotational velocities for nine primary, eight secondary, and one tertiary components of these systems were determined for the first time. The rotational velocities for primary components of seven systems appeared to be significantly different than the corresponding synchronous values (more than twice as fast for five systems, and less than half as fast for two systems). Our velocities for AU Mon, RY Gem, and RZ Eri are significantly lower than the previously published values obtained by using one or very few lines. We show that these discrepancies can be explained by strong blending of the lines in the spectra of the primaries with strong lines of the secondaries, by influence of gaseous streams, and maybe by nonsolar chemical compositions.

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Section: Introductionmentioning

confidence: 92%

Rotational Velocities of the Components of 23 Binaries

Glazunova

Yushchenko

Tsymbal

et al. 2008

The Astronomical Journal

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“…This latter problem may be overcome by high‐resolution spectroscopic observations that could reveal the Rossiter–McLaughlin effect and infer a spin axis from it, as was done for DI Herculis (Albrecht et al 2009). The effect has already been detected in RZ Cas (Lehmann & Mkrtichian 2008), and the possibility is open for other cases as well.…”

Section: Discussionmentioning

confidence: 83%

Photometric mode identification methods of non-radial pulsations in eclipsing binaries - I. Dynamic eclipse mapping

Bíró¹,

Nuspl

2011

Monthly Notices of the Royal Astronomical Society

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We present the dynamic eclipse mapping method designed specifically to reconstruct the surface intensity patterns of non‐radial stellar oscillations on components of eclipsing binaries. The method needs a geometric model of the binary, accepts the light curve and the detected pulsation frequencies on input, and on output yields estimates of the pulsation patterns, in the form of images, thus allowing a direct identification of the surface mode numbers (ℓ, m). Since it has minimal modelling requirements and can operate on photometric observations in arbitrary wavelength bands, dynamic eclipse mapping is well suited to analyse the wide‐band time series collected by space observatories. We have investigated the performance and the limitations of the method through extensive numerical tests on simulated data, in which almost all photometrically detectable modes with a latitudinal complexity ℓ− |m| ≤ 4 were properly restored. The method is able by its nature to simultaneously reconstruct multimode pulsations from data covering a sufficient number of eclipses as well as pulsations on components with a tilted rotation axis of a known direction. It can also be applied in principle to isolate the contribution of hidden modes from the light curve. Sensitivity tests show that moderate errors in the geometric parameters and the assumed limb darkening can be partially tolerated by the inversion, in the sense that the lower degree modes are still recoverable. Tidally induced or mutually resonant pulsations, however, are an obstacle that neither the eclipse mapping nor any other inversion technique can ever surpass. We conclude that, with reasonable assumptions, dynamic eclipse mapping could be a powerful tool for mode identification, especially in moderately close eclipsing binary systems, where the pulsating component is not seriously affected by tidal interactions so that the pulsations are intrinsic to them, and not a consequence of the binarity.

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“…Because of the possible existence of a complex pulsational behaviour as well as of amplitude variability in such oscillating Algol-type stars (e.g. RZ Cas, Lehmann and Mkrtichian 2008;Y Cam, Rodríguez et al 2007), it is important to perform various checks in order to confirm the absence of any pulsation at different epochs and possibly in different mass transfer regimes.…”

Section: Search For Possible Pulsation(s)mentioning

confidence: 99%

The Algol-type eclipsing binaries RW CrB and VZ Leo: new RI photometric study and search for pulsations

Ulaş

Niarchos²,

Lampens

et al. 2008

Astrophys Space Sci

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In this study we present the new R and I light curve solutions for the eclipsing binary systems RW CrB and VZ Leo, which for VZ Leo is the first one in the literature. Our new observations have been analyzed using the Wilson-Devinney code from which new geometric and photometric elements are derived. The geometry of both stars is that of a semi-detached binary system where the secondary component fills its Roche lobe while the primary component is well inside. In the case of RW CrB, asymmetry in the light curve was explained by a spot model. The orbital period changes of both systems were studied and the results indicated a period decrease which can be explained by angular momentum loss. We also investigated the possibility of pulsations of the primary components since these systems are mentioned as candidates of δ Sct type pulsation. However, a time-series analysis of the residual curves in the filter I does not indicate any evidence of periodic light variation for both systems. Finally, we compared the results obtained for both binary stars to those of similar systems.

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The eclipsing binary star RZ Cassiopeiae

Cited by 16 publications

References 19 publications

Rotational Velocities of the Components of 23 Binaries

Rotational Velocities of the Components of 23 Binaries

Photometric mode identification methods of non-radial pulsations in eclipsing binaries - I. Dynamic eclipse mapping

The Algol-type eclipsing binaries RW CrB and VZ Leo: new RI photometric study and search for pulsations

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