The eclipsing binary star RZ Cas: accretion-driven variability of the multimode oscillation spectrum

Mkrtichian, D. E.; Lehmann, H.; Rodríguez‐López, C.; Olson, Edward C.; Kim, S. L.; Kusakin, A.; Lee, J. W.; Youn, Jae-Hyuck; Kwon, S. G.; López-González, M. J.; Janiashvili, E. B.; Tiwari, S. K.; Joshi, Santosh; Lampens, P.; Cauteren, P. van; Glazunova, L. V.; Gamarova, A. Yu.; Grankin, K. N.; Rovithis‐Livaniou, Eleni; Svoboda, Petr; Uhlàř, R.; Tsymbal, V.; Kokumbaeva, R. I.; Urushadze, T.; Kuratov, K. S.; Shin, Hak-Ki; Kang, Yong; Soonthornthum, Boonrucksar

doi:10.1093/mnras/stx2841

Cited by 24 publications

(29 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Amplitude modulation of pulsation modes both during the orbital phase and on time scales of hundreds to thousands of days has been inferred in some oEA stars using ground-based data (e.g. RZ Cas; Mkrtichian et al 2018). Accretion-driven variability and variable extinction within the semi-transparent circumbinary environment is plausibly the cause of long-term amplitude variability in U Gru, as has been inferred for other oEA systems (e.g.…”

Section: The Pulsating Eclipsing Binary U Gru -Tic 147201138mentioning

confidence: 64%

Discovery of Tidally Perturbed Pulsations in the Eclipsing Binary U Gru: A Crucial System for Tidal Asteroseismology

Bowman

Johnston

Tkachenko

et al. 2019

ApJL

View full text Add to dashboard Cite

The interior physics of stars is currently not well constrained for early-type stars. This is particularly pertinent for multiple systems as binary interaction becomes more prevalent for more massive stars, which strongly affects their evolution. High-precision photometry from the Transiting Exoplanet Survey Satellite (TESS) mission offers the opportunity to remedy the dearth of observations of pulsating stars that show evidence of binary interaction, specifically pulsating mass-accreting components of semidetached Algol-type eclipsing binary (oEA) systems. We present the TESS light curve of the circular eclipsing binary system U Gru (TIC 147201138), which shows evidence for free heat-driven pressure modes and a series of tidally-perturbed pressure modes. We highlight the asteroseismic potential of studying pulsating stars in binary systems, and demonstrate how tidal asteroseismology can be applied to infer the influence of binary interaction on stellar structure.

show abstract

Section: The Pulsating Eclipsing Binary U Gru -Tic 147201138mentioning

confidence: 64%

Discovery of Tidally Perturbed Pulsations in the Eclipsing Binary U Gru: A Crucial System for Tidal Asteroseismology

Bowman

Johnston

Tkachenko

et al. 2019

ApJL

View full text Add to dashboard Cite

show abstract

“…KIC 4544587 is a short-period EB with self-excited pressure (p) and gravity (g) modes, tidally excited (g) modes, as well as tidally perturbed (p) modes. Although the system is a short-period though eccentric binary, no sign of activity was reported and no process (episodes) of mass transfer was considered (as occurred in, e.g., RZ Cas [38]). In order to explain both the eccentricity and the fast apsidal motion, the authors suggest the presence of (extreme) tidal interactions or an (undetected) companion.…”

Section: Conclusion-discussionmentioning

confidence: 99%

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Lampens

2021

Galaxies

View full text Add to dashboard Cite

Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) mass transfer between the components and/or magnetic activity. How these phenomena and the orbital changes affect the different types of pulsations excited in one or more components, offers a new window of opportunity to better understand the physics of pulsations.

show abstract

“…However, it could also be caused by an amplification of observed oscillations from non-radial pulsation modes of special l, m combinations due to the eclipse mapping effect. This effect, also called the spatial filtration effect, was described by Gamarova et al (2003) and Mkrtichian et al (2005) as a tool for the identification of non-radial pulsation modes and applied to the oEA stars AB Cas (Rodríguez et al 2004a) and RZ Cas (Gamarova et al 2003;Mkrtichian et al 2018). It is based on the fact that the surface of the pulsating component is scanned during primary eclipse by its companion which works as a timely variable spatial filter causing specific changes in the pulsation light curve and also in the observed line profiles.…”

Section: Search For Short-term Variationsmentioning

confidence: 99%

“…The best investigated object among the oEA stars is RZ Cas (e.g. Lehmann & Mkrtichian 2004, 2008Rodríguez et al 2004b;Soydugan et al 2006;Tkachenko et al 2009;Mkrtichian et al 2018). Mkrtichian & Gamarova (2000) reported on low-amplitude acoustic mode oscillations in the light curve of R CMa with a frequency of 21.21 c d −1 .…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic time-series analysis of R Canis Majoris

Lehmann

Tsymbal

Pertermann

et al. 2018

A&A

View full text Add to dashboard Cite

R Canis Majoris is the prototype of a small group of Algol-type stars showing short orbital periods and low mass ratios. A previous detection of short-term oscillations in its light curve has not yet been confirmed. We investigate a new time series of high-resolution spectra with the aim to derive improved stellar and system parameters, to search for the possible impact of a third component in the observed spectra, to look for indications of activity in the Algol system, and to search for short-term variations in radial velocities. We disentangled the composite spectra into the spectra of the binary components. Then we analysed the resulting high signal-tonoise spectra of both stars. Using a newly developed program code based on an improved method of least-squares deconvolution, we were able to determine the radial velocities of both components also during primary eclipse. This allowed us to develop a better model of the system including the Rossiter-McLaughlin effect and to derive improved orbital parameters. Combining the results with those from spectrum analysis, we obtain accurate stellar and system parameters. We further deduce at least one oscillation frequency of 21.38 c d −1 . It could be detected during primary eclipses only and confirms a previous photometric finding. Results point to an amplitude amplification of non-radial pulsation modes due to the eclipse mapping effect. The presence of a He I line in the spectra indicates mass transfer in the R CMa system. Calculations of its Roche geometry give evidence that the cool secondary component may fill its Roche lobe. No evidence of a third body in the system could be found in the observed spectra.

show abstract

The eclipsing binary star RZ Cas: accretion-driven variability of the multimode oscillation spectrum

Cited by 24 publications

References 61 publications

Discovery of Tidally Perturbed Pulsations in the Eclipsing Binary U Gru: A Crucial System for Tidal Asteroseismology

Discovery of Tidally Perturbed Pulsations in the Eclipsing Binary U Gru: A Crucial System for Tidal Asteroseismology

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Spectroscopic time-series analysis of R Canis Majoris

Contact Info

Product

Resources

About