The eclipsing binary star RZ Cas

Lehmann, H.; Mkrtichian, D. E.

doi:10.1051/0004-6361:20031503

Cited by 27 publications

(30 citation statements)

References 11 publications

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“…Only one pulsation frequency, being about 64.19 cd −1 , had been obtained up to 2000. On the other hand, spectroscopic observations made in 2001 showed the existence of at least two close frequencies with the values of 56.6 cd −1 and 64.189 cd −1 (Lehmann & Mkrtichian 2004). …”

Section: Introductionmentioning

confidence: 88%

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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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Section: Introductionmentioning

confidence: 88%

“…d 1953 and a δ Scuti-type primary component (Ohshima et al 1998(Ohshima et al , 2001; Lehmann & Mkrtichian 2004;Rodriguez et al 2004) . The spectral types of the primary and the secondary components are A3V and K0IV, respectively.…”

Section: Introductionmentioning

confidence: 99%

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

Soydugan

İbanoǧlu

et al. 2006

Astron. Nachr.

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“…In fact, radial and nonradial pulsation modes detected in both, photometric and spectroscopic observations for other spectral types, indicate that a signal of 10 µmag can have a counterpart of 1 m s −1 in RVs (e.g. δ Scuti and γ Dor oscillators such as FG Vir, RZ Cas, 9-Aur, HR 8799, gam Dor, and HD 49434; Zima et al 2006;Lehmann & Mkrtichian 2004;Zerbi et al 1997Zerbi et al , 1999Krisciunas et al 1995;Uytterhoeven et al 2008); an amplitude that is detectable with HARPS-ESO, which has a reported RV precision in the short-term of 0.5 m s −1 (Lovis & Fischer 2010).…”

Section: E-mail: Zaira@iaaesmentioning

confidence: 99%

High-cadence spectroscopy of M-dwarfs – II. Searching for stellar pulsations with HARPS

Berdiñas

Rodríguez‐López

Amado

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Stellar oscillations appear all across the Hertzsprung-Russell diagram. Recent theoretical studies support their existence also in the atmospheres of M dwarfs. These studies predict for them short periodicities ranging from 20 min to 3 h. Our Cool Tiny Beats (CTB) programme aims at finding these oscillations for the very first time. With this goal, CTB explores the short time domain of M dwarfs using radial velocity data from the HARPS-ESO and HARPS-N high-precision spectrographs. Here we present the results for the two most long-term stable targets observed to date with CTB, GJ 588 and GJ 699 (i.e. Barnard's star). In the first part of this work we detail the correction of several instrumental effects. These corrections are specially relevant when searching for sub-night signals. Results show no significant signals in the range where M dwarfs pulsations were predicted. However, we estimate that stellar pulsations with amplitudes larger than ∼ 0.5 m s −1 can be detected with a 90% completeness with our observations. This result, along with the excess of power regions detected in the periodograms, open the possibility of non-resolved very low amplitude pulsation signals. Next generation more precise instrumentation would be required to detect such oscillations. However, the possibility of detecting pulsating M-dwarf stars with larger amplitudes is feasible due to the short size of the analysed sample. This motivates the need for completeness of the CTB survey.

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“…Also, accretion in an interacting binary might be studied via the RM effect (e.g. Lehmann & Mkrtichian 2004).…”

Section: Introductionmentioning

confidence: 99%