Tidally Excited Modes and δ Scuti Pulsations in the Eclipsing Triple Star IM Persei

Lee, Jae Woo; Hong, Kyeongsoo; Kim, Hye-Young

doi:10.3847/1538-3881/abd631

Cited by 10 publications

(8 citation statements)

References 27 publications

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“…The light curve of this eclipsing binary system has been recently studied by Lee et al (2021) using TESS measurements. An eccentricity e = 0.0305 ± 0.0009, with an argument of periastron ω = 212.7 ± 3.2 deg were obtained from the analysis.…”

Section: -Cw Cepmentioning

confidence: 99%

Analysis of apsidal motion in eclipsing binaries using TESS data

Claret

Giménez

Baroch

et al. 2021

A&A

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Context. The measurement of apsidal motion rates in eccentric eclipsing binaries is a unique way to gain insight into the internal structure of stars through the internal density concentration parameter, k2. High-quality physical parameters of the stellar components, together with precise measurements of the advance of the periastron, are needed for the comparison with values derived from models. Aims. As a product of the Transiting Exoplanet Survey Satellite (TESS) mission, high-precision light curves of a large number of eclipsing binaries are now available. Using a selection of well-studied, double-lined eccentric eclipsing binary systems, we aim to determine their apsidal motion rates and place constraints on the internal density concentration and compare with the predictions from state-of-the-art theoretical models. Methods. We computed times of minimum light using the TESS light curves of 34 eclipsing binaries with precise absolute parameters. We used the changing difference over time between primary and secondary eclipse timings to determine the apsidal motion rate. To extend the time baseline, we combined the high-precision TESS timings with reliable archival data. On the other hand, for each component of our sample of double-lined eclipsing binaries, we computed grids of evolutionary stellar models for the observed stellar mass exploring ranges of values of the overshooting parameter fov, the mixing-length parameter, and the metallicity. To find the best solution for the two components we adopted a χ2 statistic to infer the optimal values of the overshooting parameter and the mixing-length parameter. The theoretical internal structure constants to be compared with the observed values were calculated by integrating the differential equations of Radau for each stellar model. Results. We have determined the apsidal motion rate of 27 double-lined eclipsing binaries with precise physical parameters. The obtained values, corrected for their relativistic contribution, yield precise empirical parameters of the internal stellar density concentration. The comparison of these results with the predictions based on new theoretical models shows very good agreement. Small deviations are identified but remain within the observational uncertainties and the path for a refined comparison is indicated.

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Section: -Cw Cepmentioning

confidence: 99%

Analysis of apsidal motion in eclipsing binaries using TESS data

Claret

Giménez

Baroch

et al. 2021

A&A

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“…With the TESS measurements of T 2 − T 1 in different sectors, apsidal motion is already evident and we determine a slope of (2.8 ± 0.2) × 10 −5 days/cycle over a time span of 70 orbital cycles. We have added the T 2 − T 1 values retrieved from the literature to compute the corresponding argument of periastron with the orbital eccentricity given by Lee et al (2021). We have restricted eclipse timings to those obtained by means of photoelectric measurements and considered pairs within less than 10 orbital cycles.…”

Section: -Cw Cepmentioning

confidence: 99%

Analysis of apsidal motion in eclipsing binaries using TESS data II. A test of internal stellar structure}

Claret,

Giménez,

Baroch

et al. 2021

Preprint

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Context. The measurement of apsidal motion rates in eccentric eclipsing binaries is a unique way to gain insight into the internal structure of stars through the internal density concentration parameter, k 2 . High-quality physical parameters of the stellar components, together with precise measurements of the advance of the periastron, are needed for the comparison with values derived from models. Aims. As a product of the Transiting Exoplanet Survey Satellite (TESS) mission, high-precision light curves of a large number of eclipsing binaries are now available. Using a selection of well-studied, double-lined eccentric eclipsing binary systems, we aim to determine their apsidal motion rates and place constraints on the internal density concentration and compare with the predictions from state-of-the-art theoretical models. Methods. We computed times of minimum light using the TESS light curves of 34 eclipsing binaries with precise absolute parameters. We used the changing difference over time between primary and secondary eclipse timings to determine the apsidal motion rate. To extend the time baseline, we combined the high-precision TESS timings with reliable archival data. On the other hand, for each component of our sample of double-lined eclipsing binaries, we computed grids of evolutionary stellar models for the observed stellar mass exploring ranges of values of the overshooting parameter f ov , the mixing-length parameter, and the metallicity. To find the best solution for the two components we adopted a χ 2 statistic to infer the optimal values of the overshooting parameter and the mixinglength parameter. The theoretical internal structure constants to be compared with the observed values were calculated by integrating the differential equations of Radau for each stellar model. Results. We have determined the apsidal motion rate of 27 double-lined eclipsing binaries with precise physical parameters. The obtained values, corrected for their relativistic contribution, yield precise empirical parameters of the internal stellar density concentration. The comparison of these results with the predictions based on new theoretical models shows very good agreement. Small deviations are identified but remain within the observational uncertainties and the path for a refined comparison is indicated.

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“…Lee et al [294] also determined the masses and radii of the stars and detected slow apsidal motion. The triple system IM Per has been found to show δ Scuti, γ Dor and tidally-perturbed oscillations in TESS data (Lee et al [296]), as has RR Lyn (Southworth,[297]). An important recent result for δ Scuti pulsations is the discovery of regular sequences of oscillations in young stars which enable clear mode identification [298].…”

Section: Pulsatorsmentioning

confidence: 98%

Space-Based Photometry Of Binary Stars: From Voyager To TESS

Southworth¹

2021

Preprint

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Binary stars are crucial laboratories for stellar physics, so have been photometric targets for space missions beginning with the very first orbiting telescope (OAO-2) launched in 1968. This review traces the binary stars observed and the scientific results obtained from the early days of ultraviolet missions (OAO-2, Voyager, ANS, IUE), through a period of diversification (Hipparcos, WIRE, MOST, BRITE), to the current era of large planetary transit surveys (CoRoT, Kepler, TESS). In this time observations have been obtained of detached, semi-detached and contact binaries containing dwarfs, sub-giants, giants, supergiants, white dwarfs, planets, neutron stars and accretion discs. Recent missions have found a huge variety of objects such as pulsating stars in eclipsing binaries, multi-eclipsers, heartbeat stars and binaries hosting transiting planets. Particular attention is paid to eclipsing binaries, because they are staggeringly useful, and to the NASA Transiting Exoplanet Survey Satellite (TESS) because its huge sky coverage enables a wide range of scientific investigations with unprecedented ease. These results are placed into context, future missions are discussed, and a list of important science goals is presented.

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Tidally Excited Modes and δ Scuti Pulsations in the Eclipsing Triple Star IM Persei

Cited by 10 publications

References 27 publications

Analysis of apsidal motion in eclipsing binaries using TESS data

Analysis of apsidal motion in eclipsing binaries using TESS data

Analysis of apsidal motion in eclipsing binaries using TESS data II. A test of internal stellar structure}

Space-Based Photometry Of Binary Stars: From Voyager To TESS

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