First apsidal motion and light curve analysis of 162 eccentric eclipsing binaries from LMC

Zasche, P.; Wolf, M.; Kučáková, H.; Kára, Jan; Merc, Jaroslav; Zejda, Miloslav; Skarka, Marek; Janík, Ján; Kurfürst, Petr

doi:10.1051/0004-6361/202037822

Cited by 6 publications

(1 citation statement)

References 31 publications

(33 reference statements)

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“…5) match the morphology of their light curves obtained by the OGLE team. Some differences for EB#1 can be explained by the apsidal motion in this system (Zasche et al 2020). Both systems are relatively bright (V = 15.8 and 15.6 mag, respectively), which explains why they contaminate the light curve of the ExtEEV.…”

Section: Analysis Of the Tess Light Curvementioning

confidence: 88%

Tidally excited oscillations in MACHO 80.7443.1718: Changing amplitudes and frequencies, high-frequency tidally excited mode, and a decrease in the orbital period

Kołaczek-Szymański

Pigulski

Wrona

et al. 2022

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Context. Eccentric ellipsoidal variables (also known as heartbeat stars) is a class of eccentric binaries in which proximity effects, and tidal distortion due to time-dependent tidal potential in particular, lead to measurable photometric variability close to the periastron passage. Varying tidal potential may also give rise to tidally excited oscillations (TEOs), which are forced eigenmodes with frequencies close to the integer multiples of the orbital frequency. TEOs may play an important role in the dynamical evolution of massive eccentric systems. Aims. Our study is aimed at detecting TEOs and characterising the long-term behaviour of their amplitudes and frequencies in the extreme-amplitude heartbeat star MACHO 80.7443.1718, consisting of a blue supergiant and a late O-type massive dwarf. Methods. We used two seasons of Transiting Exoplanet Survey Satellite (TESS) observations of the target to obtain new 30-min cadence photometry by means of the difference image analysis of TESS full-frame images. In order to extend the analysis to longer timescales, we supplemented the TESS data with 30-year long ground-based photometry of the target. Both TESS and ground-based photometry are carefully analysed by means of Fourier techniques in order to detect TEOs, examine the long-term stability of their amplitudes and frequencies, and characterise other types of variability in the system. Results. We confirm the detection of the known n = 23, 25, and 41 TEOs and announce the detection of two new TEOs, with n = 24 and 230, in the photometry of MACHO 80.7443.1718. Amplitudes of all TEOs were found to vary on a timescale of years or months. For n = 25, the TEO amplitude and frequency changes are related, which may indicate that the main cause of the amplitude drop in this TEO in TESS observations is the change in its frequency and increase in its detuning parameter. The light curve of the n = 230 TEO is strongly non-sinusoidal. Its high frequency may indicate that the oscillation is a strange mode. Stochastic variability observed in the target fits the behaviour observed in massive stars well and independently confirms that the primary is an evolved star. We also find that the orbital period of the system decreases at a rate of about 11 s (yr)−1. This can be explained by several phenomena: a significant mass loss, mass transfer between components, tidal dissipation, and the presence of a tertiary in the system. All of these phenomena may contribute to the observed changes. Conclusions. The discovery of variable amplitudes and frequencies of TEOs prompts for similar studies in other eccentric elliptical variables with TEOs. Long-term photometric monitoring of these targets is also desirable. The results we obtained pose a challenge for theory. In particular, it needs to be explained why n = 230 TEO is excited. In a general context, studies on the long-term behaviour of TEOs may help to explain the role of TEOs in the dynamical evolution of massive eccentric systems.

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Section: Analysis Of the Tess Light Curvementioning

confidence: 88%

Tidally excited oscillations in MACHO 80.7443.1718: Changing amplitudes and frequencies, high-frequency tidally excited mode, and a decrease in the orbital period

Kołaczek-Szymański

Pigulski

Wrona

et al. 2022

A&A

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The two eccentric eclipsing binaries in multiple systems: V539 Arae and V335 Serpentis

et al. 2022

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Theoretical tidal evolution constants for stellar models from the pre-main sequence to the white dwarf stage

Claret¹

2023

A&A

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Aims. One of the most reliable means of studying the stellar interior is through the apsidal motion in double line eclipsing binary systems since these systems present errors in masses, radii, and effective temperatures of only a few per cent. On the other hand, the theoretical values of the apsidal motion to be compared with the observed values depend on the stellar masses of the components and more strongly on their radii (fifth power). The main objective of this work is to make available grids of evolutionary stellar models that, in addition to the traditional parameters (e.g. age, mass, log g, Teff), also contain the necessary parameters for the theoretical study of apsidal motion and tidal evolution. This information is useful for the study of the apsidal motion in eclipsing binaries and their tidal evolution, and can also be used for the same purpose in exoplanetary systems. Methods. All models were computed using the MESA package. We consider core overshooting for models with masses ≥1.2M⊙. For the amount of core overshooting we adopted a recent relationship for mass × core overshooting. We adopted for the mixing-length parameter αMLT the value 1.84 (the solar-calibrated value). Mass loss was taken into account in two evolutionary phases. The models were followed from the pre-main sequence phase to the white dwarf (WD) stage. Results. The evolutionary models containing age, luminosity, log g, and Teff, as well as the first three harmonics of the internal stellar structure (k2, k3, and k4), the radius of gyration βy, and the dimensionless variable α, related to gravitational potential energy, are presented in 69 tables covering three chemical compositions: [Fe/H] = −0.50, 0.00, and 0.50. Additional models with different input physics are available.

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First apsidal motion and light curve analysis of 162 eccentric eclipsing binaries from LMC

Cited by 6 publications

References 31 publications

Tidally excited oscillations in MACHO 80.7443.1718: Changing amplitudes and frequencies, high-frequency tidally excited mode, and a decrease in the orbital period

Tidally excited oscillations in MACHO 80.7443.1718: Changing amplitudes and frequencies, high-frequency tidally excited mode, and a decrease in the orbital period

The two eccentric eclipsing binaries in multiple systems: V539 Arae and V335 Serpentis

Theoretical tidal evolution constants for stellar models from the pre-main sequence to the white dwarf stage

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