The first study of 54 new eccentric eclipsing binaries in our Galaxy

Zasche, P.; Wolf, M.; Uhlàř, R.; Cagaš, P.; Jurýšek, Jakub; Mašek, M.; Hoňková, K.; Kučáková, H.; Lehký, M.; Kotková, L.; White, G. J.; Bewsher, D.; Tylšar, M.; Jelínek, M.; Paschke, A.

doi:10.1051/0004-6361/201832793

Cited by 9 publications

(7 citation statements)

References 40 publications

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“…This implies -see, e.g., Winn 2010e cos ω = π∆T 2P orb = 0.005 ± 0.001, where the error has been estimated from the error of the average ∆T . Third, the period of the sinusoidal component of the O-C variation of our target is relatively short, and therefore, not too common among objects showing apsidal motion (see Hong et al 2016 andZasche et al 2018).…”

Section: Physical Interpretationmentioning

confidence: 94%

The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

Kovács

Hartman

Bakos

2019

A&A

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We revisit the issue of period variation of the recently claimed red nova precursor candidate KIC 9832227. By using the data gathered during the main mission of the Kepler satellite, those collected by ground-based wide-field surveys and other monitoring programs (such as ASAS-SN), we find that the currently available timing data strongly support a model consisting of the known W UMa binary and a distant low-mass companion with an orbital period of ∼ 13.5 years. The period of the W UMa component exhibits a linear period decrease with a pace of (1.10 ± 0.05) × 10 −6 days per year, within the range of many other similar systems. This rate of decrease is several orders of magnitude lower than that of V1309 Sco, the first (and so far the only) well-established binary precursor of a nova observed a few years before the outburst. The high-fidelity fit of the timing data and the conformity of the derived minimum mass of (0.38 ± 0.02) M ⊙ of the outer companion from these data with the limit posed by the spectroscopic non-detection of this component, are in agreement with the suggested hierarchical nature of this system.

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Section: Physical Interpretationmentioning

confidence: 94%

The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

Kovács

Hartman

Bakos

2019

A&A

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“…The system was first identified as an eccentric eclipsing system with a correct orbital period by Martignoni (2013). The system was included in our previous study (Zasche et al 2018), where we used the poor photometric data from the discovery paper and no spectroscopy. In that study a very slow rate of apsidal motion and an eccentricity of 0.32 were derived for the system.…”

Section: Tyc 5378-1590-1mentioning

confidence: 99%

“…Using all available photometric data for the star TYC 5378-1590-1, we also performed a period analysis using the longest possible time interval. The data added to those used in our former study (Zasche et al 2018) were primarily composed of the TESS observations, supplemented by more recent ASAS-SN data. However, our results indicate only a slight evolution of the apsidal angle ω, meaning that the apsidal motion occurs at a very slow rate (on the order of thousands of years).…”

Section: Tyc 5378-1590-1mentioning

confidence: 99%

“…TYC 8378-252-1 (= ASAS J185951-4711.8, RA 18 h 59 m 51.29 s DE -47 • 11 ′ 47.59 ′′ , V = 11.2 mag) has been mentioned only briefly as an eclipsing binary system in prior work based on survey data from CRTS and ASAS. It was also included in our previous study (Zasche et al 2018), where we derived an eccentricity of e = 0.167 for its orbit, and slow apsidal motion with U = 558 yr. A more detailed analysis of this star has not been published to date.…”

Section: Tyc 8378-252-1mentioning

confidence: 99%

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First detailed study of two eccentric eclipsing binaries: TYC 5378-1590-1 and TYC 8378-252-1

Zasche

Sürgit

Erdem

et al. 2023

A&A

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Aims: The analysis of combined photometry and spectroscopy of eccentric eclipsing binary systems facilitates the derivation of very precise values for a large ensemble of physical parameters of the component stars and their orbits, thereby providing stringent tests of theories of stellar structure and evolution. In this paper two eccentric eclipsing binary systems, TYC 5378-1590-1 and TYC 8378-252-1, are studied in detail for the first time. Methods: Radial velocities were obtained using cross-correlation methods applied to mid-resolution spectra covering almost the entire orbital phase domains of these two systems. TESS photometry was used for the analysis of TYC 5378-1590-1, whereas ASAS-SN photometry was used for the analysis of TYC 8378-252-1. Results: We obtained the first precise derivation of the physical parameters of these systems. Both systems display moderately eccentric orbits (e ∼ 0.3 and 0.2) with periods of 3.73235 and 2.87769 days, respectively. The apsidal motion is very slow, with a duration of several centuries for both systems. We present two models for the apsidal motion of TYC 5378-1590-1. The internal structure constant derived from observations for TYC 8378-252-1 is approximately 11% lower than theoretical predictions. We discuss possible reasons for this discrepancy. Our analysis indicates that the components of both systems are on the main sequence. The components of TYC 5378-1590-1 are relatively young stars (age ∼ 600 Myr) close to the ZAMS, whereas the components of TYC 8378-252-1 are relatively old stars (age ∼ 4 Gyr) close to the TAMS. Our finding that the circularization timescale for TYC 5378-1590-1 is ∼ 200 times longer than its evolutionary age is compatible with circularization theory; however, our finding that the evolutionary age of TYC 8378-252-1 is approximately ten times longer than the circulation age, while its orbital eccentricity is quite high (e ∼ 0.2), challenges the present theories of circularization.

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“…The light elements of V839 Cep (GSC 3964-0741) were given by Otero et al (2006) as T 0 (HJD) = 2451448.645 and period P = 9.9634 d. Detailed apsidal motion studies were performed by Zasche et al (2018) and Volkov et al (2019). Here we derive absolute parameters of the system.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic observations of eccentric eclipsing binary systems

Kiran¹,

Bakış²,

Bakıș³

2020

caosp

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Eccentric eclipsing binaries (EEBs) are detached binary stars. Many EEBs show apsidal motion. EEB fundamental physical parameters allow us to test stellar evolution models and to estimate the internal stellar structure constants through apsidal motion analysis. We started a programme to study EEBs at the UBT60 telescope of Akdeniz University located at TÜBİTAK National Observatory. In this paper, we present spectroscopic orbital parameters of some selected EEBs.

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The first study of 54 new eccentric eclipsing binaries in our Galaxy

Cited by 9 publications

References 40 publications

The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

First detailed study of two eccentric eclipsing binaries: TYC 5378-1590-1 and TYC 8378-252-1

Spectroscopic observations of eccentric eclipsing binary systems

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