Mass Ratio and Spot Parameter Estimation from Eclipsing Binary Star Light Curves

Terrell, Dirk

doi:10.3390/galaxies10010008

Cited by 10 publications

(8 citation statements)

References 27 publications

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“…The relationship between the mean residual and mass ratio q is shown in Figure 1. It is clearly seen that all the q − search curves have very deep and sharp minima, indicating very precise mass ratio can be obtained (e.g., Zhang et al 2017;Li et al 2019Li et al , 2021bTerrell 2022). The mass ratio corresponding to the minimum of the mean residual was chosen as the initial value and an adjustable parameter, new solutions were started to obtain a convergent result, then the errors of mass ratio can be determined.…”

Section: Light-curve Investigationmentioning

confidence: 99%

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Gao

Liu

et al. 2022

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The photometric and spectroscopic investigations of ten contact binaries were presented for the first time. It is discovered that the mass ratios of all the ten targets are smaller than 0.15, they are extremely low mass ratio contact binaries. Seven of them are deep contact binaries, two are medium contact binaries, while only one is a shallow contact system. Five of them show the O’Connell effect, and a dark spot on one of the two components can lead to a good fit of the asymmetric light curves. The orbital period studies of the ten binaries reveal that they all exhibit long-term period changes, six of them are increasing, while the others are shrinking. The LAMOST spectra were analyzed by the spectral subtraction method, and all the ten targets exhibit excess emissions in the H α line, indicating chromospheric activity. The evolutionary states of the two components of the ten binaries were studied, and it is found that their evolutionary states are identical to those of the other contact binaries. Based on the study of the relation between orbital angular momentum and total mass, we discovered the ten systems may be at the late evolutionary stage of a contact binary. The initial masses of the two components and the ages of them were obtained. By calculating the instability parameters, we found that the ten contact binaries are relatively stable at present.

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Section: Light-curve Investigationmentioning

confidence: 99%

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Gao

Liu

et al. 2022

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“…Terrell & Wilson (2005) showed that the photometric mass ratio for semi-detached and over-contact binaries is often overestimated for partial eclipses. Recently Terrell (2022) noted that not properly modeled third light will lead to mass ratios that are too low. Our solution of RU UMi show no third light and no total eclipses on the LCs (just like other stars).…”

Section: Discussionmentioning

confidence: 99%

Photomeric analysis of eclipsing binaries: VY UMI, RU UMI AND GSC 04364-00648

Kudak¹,

Parimucha²,

Perig³

et al. 2023

Preprint

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We present the photometric analysis of BVR and TESS light curves of three eclipsing binaries (RU UMi and purely studied VY UMi, GSC 04364-00648), together with their period changes considering archival data and new minima times from our and TESS observations. For the first time we detected wave-like variations with low-amplitude in O − C residua of RU UMi, which can be interpreted as a consequence of the light-time effect caused by the 3rd invisible component with period 7370 days. Period increase with rate 2.56(9)×10 −7 d/yr −1 detected in the VY UMi system corresponds to mass transfer from the secondary to the primary component. For GSC 04364-00648 binary system we find some quadratic changes on the O − C diagram, which corresponds to a period decrease with a high rate of −2.26(5) × 10 −5 d/yr −1 . We cannot assumptions about their nature, mainly due to short time of observation and uneven coverage of O − C diagram. We also determined the absolute parameter of their components using the photometric solution and GAIA distances.

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“…We considered this model as the underlying model that can describe the system and explored the LC solution of our 2016 data with a spotted model using a GA optimizer. The GAs show promise for determining spot parameters from a simultaneous solution of LCs with broad wavelength coverage (Terrell 2022). To investigate spot parameters, the PHOEBE program was interfaced with PIKAIA.…”

Section: Lc Modelingmentioning

confidence: 99%

Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys

Παπαγεωργίου

Christopoulou

Lopes

et al. 2023

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We present the photometric analysis of three ultra-short-period total eclipsing binaries in contact configuration, CRTS_J172718.0+431624, OGLE-BLG-ECL-000104, and OGLE-BLG-ECL-000012, mined from massive astronomical surveys. Using the available archival light curves (LCs) from Vista Variables in the Vía Láctea (VVV), Optical Gravitational Lensing Experiment (OGLE), Zwicky Transient Facility, and Catalina Sky Survey in different passbands and new multiband photometric observations with the 2.3 m Aristarchos telescope at Helmos Observatory, their relative physical parameters were derived. We explored the parameter space by using the PIKAIA genetic algorithm optimizer. The best photometric solution and error budget estimation were adopted for each system through Markov Chain Monte Carlo sampling of the global optimum. The approximate absolute parameters were derived for each contact system adopting an empirical mass–luminosity relation. All three systems have a mass ratio lower than 0.5. The exchange between the primary and secondary depths of CRTS_J172718.0+431624 during 2016–2022 may be due to spot activity. In addition, we present a detailed analysis of the first well-characterized shortest-period contact eclipsing binary with total eclipses known so far (OGLE-BLG-ECL-000104). Thanks to VVV and OGLE LCs, new distances were derived for OGLE-BLG-ECL-000104 and OGLE-BLG-ECL-000012 using empirical period–luminosity relations. The origin and evolutionary status of all three ultra-short-period contact binaries are thoroughly discussed in the context of the detached binary formation channel.

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Mass Ratio and Spot Parameter Estimation from Eclipsing Binary Star Light Curves

Cited by 10 publications

References 27 publications

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Photomeric analysis of eclipsing binaries: VY UMI, RU UMI AND GSC 04364-00648

Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys

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