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19 results for “eclipsing binaries”
TESS-validated Gaia DR3 Pulsating Variables of δ Scuti and γ Doradus: II. 360+ Eclipsing Binaries with δ Scuti and γ Doradus Components
<div> <div> <div> <p>I present serendipitous discoveries of 380 eclipsing binaries with δ Scuti and γ Doradus pulsators, 46 eclipsing binaries exhibiting rotational variability, and 8 new RR Lyrae stars, identified for the first time during a validation project of pulsating variables from Gaia Data Release 3. Gaia DR3 Part 4 Variability released 12.4 million variables, including 748,058 pulsating variable stars of `DSCT|GDOR|SXPHE' types among the variability classification results of all classifiers -- 9,976,881 objects (in the file vclassre.dat, https://cdsarc.cds.unistra.fr/viz-bin/cat/I/358}). Among 75,369 analyzed stars, I confirmed 12,145 δ Scuti stars (including 8,710 new) and 8,192 γ Doradus stars (including 7,531 new). This work has significantly expanded the bona fide DSCT and GDOR catalogs to include 98,968 and 19,466 stars, respectively, providing a valuable resource for future studies. The discovery of the remarkable number of pulsating binaries underscores the significance of this project in validating Gaia’s variable star catalog. </p> </div> </div> </div> <p>The attached CSV files report the current validation results. If you use any data from the catalogs in your research, I appreciate your citation to the paper: </p> <p><strong>Zhou, A.-Y., 2024, Research Notes of the AAS, Volume 8, Number 4, 110 (ADS bibcode: 2024RNAAS...8..110Z) </strong></p> <ul> <li>CSV file GaiaDR3_vari_DSCTgDorSXPhe_Validated_R2_NewEB_Pul.csv for the newly identified Eclipsing Binaries with Pulsating components;</li> <li>CSV file GaiaDR3_vari_DSCTgDorSXPhe_Validated_R2.csv for the entire validated and newly identified results from 75,369 analyzed samples.</li> </ul> <p>This is a developing story. Check back for updates.</p>
Variability Census of Legacy Catalogs: New Pulsating Variables and Eclipsing Binaries
<div> <p>I present the preliminary results of a comprehensive variability census of the four legacy catalogs: BD (+CD+SD), HD, SAO, and PPM. This dedicated survey project aims to identify bright A-F type variable stars using high-precision space photometry from the Transiting Exoplanet Survey Satellite (TESS ) and Gaia. Phases I through V of this survey, encompassing analyses of 193,940 A-F stars selected from the aforementioned catalogs, have been completed. To date, the project has yielded a substantial number of new variable star discoveries, including: over 14,510 new δ Scuti stars, more than 18,382 new γ Doradus stars, and over 2,354 new eclipsing binary systems, with approximately 360 binaries exhibiting pulsations in the primary components. Furthermore, thousands of rotational variables and dozens of Heartbeat stars and RR Lyrae stars have been identified, demonstrating the power of this systematic approach in revealing the rich diversity of stellar variability. Due to potential blending and contamination in TESS photometry, the binarity of a few pulsating stars or those eclipsing binaries exhibiting superimposed intrinsic pulsations of <em>δ</em> Scuti and <em>γ</em> Doradus types should be rechecked. Follow-up studies of individual systems are necessary to resolve contamination issues and accurately identify the true source of variability.</p> <p> </p> </div> <div> <p>The full list of newly identified variable stars is presented in machine-readable format in the attached file `PPM_AFstars_NewVar_R5.csv', and an atlas of selected representative light curves is provided as a separate PDF.</p> </div> <p> </p> <p><strong>Citation:</strong> Zhou, Ai-Ying: 2023, <em>Res. Notes AAS,</em> Vol.<strong>7, </strong> 210 (I)</p> <p> Zhou, Ai-Ying: 2024, <em>Res. Notes AAS,</em> Vol.<strong>8, </strong> 81 (II)</p> <p> Zhou, Ai-Ying: 2024, <em>Res. Notes AAS,</em> Vol.<strong>8, </strong> 190 (III)</p> <p> Zhou, Ai-Ying: 2025, <em>Res. Notes AAS,</em> Vol.<strong>9, </strong> 56 (IV)</p> <p> Zhou, Ai-Ying: 2025, <em>Res. Notes AAS,</em> Vol.<strong>9, </strong> 1?? (V)</p>
Supplementary material for the paper "DS Andromedae, A Detached Eclipsing Double-Lined Spectroscopic Binary in the Galactic Cluster NGC 752
<p>Supplementary material supporting the paper "DS Andromedae: A Detached Eclipsing Double-Lined Spectroscopic</p> <p>Binary in the Galactic Cluster NGC 752" by E. F. Milone, S. J. Schiller, Th. Mellergaard Amby, and S. Frandsen.</p> <p>It includes:</p> <p>A Read-me file in three formats (docx, rtf, pdf); Unabridged Section 3 with extended modeling details (pdf);</p> <p>Extended spreadsheet version of Table 3 of adjusted parameters (pdf); Extended spreadsheet version of Table 8 of absolute</p> <p>parameters (pdf); and Complete Table 15 of photometric data (txt): and a sample DC input file (for Model 41, used in the</p> <p>DS And modeling) in dat format.</p>
Catalogs of Eclipsing Binaries with Pulsating Components, δ Scuti stars and γ Doradus stars
<p>I present a comprehensive, up-to-date catalog of <strong>3324</strong> <strong>eclipsing binary star systems containing pulsating components </strong>(not updated in this version). The initial compilation builds upon existing lists of `oscillating Algol-type eclipsing binaries' (oEA) harboring δ Scuti stars. However, the catalog expands upon this foundation to encompass a broader range of pulsating binary systems identified in recent years. This new catalog is valuable for researchers studying binary stars' evolution and pulsating stars. It incorporates various pulsating variable types across the Hertzsprung-Russell diagram, including δ Scuti stars, γ Doradus stars, β Cephei stars, Cepheids, and red giants exhibiting solar-like oscillations. However, this catalog is NOT an exhaustive list of eclipsing binaries with pulsating components of the above types and it is subject to updates. </p> <p>Many stars in this catalog are potentially interesting for further studies. Due to potential blending and contamination in TESS photometry, the binarity of a few pulsating stars could be attributed to neighboring eclipsing binaries. Follow-up studies of individual systems are necessary to resolve contamination issues and accurately identify the true source of variability. If you use part of the catalog in your research, please cite: Zhou, A.-Y., 2010, arXiv e-prints (DOI: 10.48550/arXiv.1002.2729) (ADS: https://ui.adsabs.harvard.edu/abs/2010arXiv1002.2729Z/abstract)</p> <p>In addition, I have also included the up-to-date catalogs of <strong>118,410 δ Scuti stars</strong> and <strong>41,622 γ Doradus stars</strong>, featuring thousands of unpublished discoveries. For these two catalogs, please cite: </p> <p>Zhou, Ai-Ying, 2024, New Astronomy, Volume 105, 102081 (Published: January 2024)</p> <p>Paper in ADS: https://ui.adsabs.harvard.edu/abs/2024NewA..10502081Z/abstract</p> <p>Paper in Publisher web: https://www.sciencedirect.com/science/article/pii/S1384107623000829</p> <p>Thanks for your reading. Your comments are more than welcome!</p>
Data for `Identifying New Pulsating Variables and Eclipsing Binaries Using TESS Data'
<p>This study presents a series of surveys using TESS data to identify new δ Scuti and γ Doradus stars, as well as eclipsing binaries with pulsating components. Preliminary catalogs of newly discovered variables are being made publicly available to encourage community use as the project progresses. Please visit this website for updates. </p> <p> 1. New δ Scuti stars, γ Doradus stars, and eclipsing binaries from a subset of 709,000 selected AF-type stars observed by TESS. Version 4.5 is an update to Version 4.0 (the first release for Part IV), while Part III was provided in Version 3.0.</p> <p> The attached CSV file <strong>NewVar_AF50w_R2.csv,</strong> contains the catalog of newly identified variables from Phases I and II of the survey (i.e. R2 includes R1 from Version 3.0). The accompanying file <strong>ms2RNAAS_2025AF50w_IV.pdf</strong> is the initial draft describing the Phase-II identifications. The published paper can be found in 2025 <em>Research Notes of the AAS</em>, <strong>Vol. 9, No. 1, 23</strong> (Zhou 2025, https://iopscience.iop.org/article/10.3847/2515-5172/adaf8c (ADS code: 2025RNAAS...9...23Z). These unpublished discoveries have been compiled into catalogs of δ Scuti and γ Doradus stars available at Zenodo https://zenodo.org/records/17096360 (DOI: <a href="https://doi.org/10.5281/zenodo.17096360">10.5281/zenodo.17096360</a>) -- which currently include <strong>118,410</strong> and <strong>41,622</strong> entries, respectively, as of the release date.</p> <p> 2. New Pulsating Variable Stars and Eclipsing Binaries around BL Cam (added in Version 2.0)</p> <p> The attached CSV file NewVar_BLCam_R2D.csv provides a catalog of the new variables with the following columns: TIC ID, Simbad main ID, Gaia DR3 ID, RA_deg Dec_deg(J2000), Tmag, Teff, SpType, Lum, logg, mass, VarType_Notes</p> <p> 3. New Pulsating Variable Stars and Eclipsing Binaries near NGC 6302 (Version 1.0)</p> <p> Check corresponding files containing the string "NGC 6302".</p>
KU Car, a young massive eclipsing binary system in NGC 3324
<p>Massive stars are needed engines in the galactic clockwork for the chemical evolution of the Galaxy and the energetic input to the ISM. These stars suffer endemic multiplicity, and thus, studies of the origin and evolution of massive stars is tied to the study of binaries. Therefore, eclipsing binary systems are indispensable objects because absolute parameters (e.g. masses, radii, etc.) can be derived combining the study and modeling of radial velocity and light curves. Such absolute parameters derived from direct observations help to test models about the structure and evolution of massive stars. In this talk, we are presenting an analysis of the light and radial velocity curves of the eclipsing binary system KU Car (P=2.96 d). This binary, composed by a B0.5-0.7 V primary and an unseen companion, shows a remarkable light-curve with a sharp and deep primary minimum and a shallow secondary minimum with strong "reflection effect". Using PHOEBE 2.1 code for modeling, we have derived absolute parameters for both stars proposed the evolutionary stage. This Algol-like system dominated by a young early-B type star, is located in the center of NGC 3324, a bubble-like star-forming region also known as "Gabriela Mistral" Nebula. The photometric analysis is based on multi-band observations obtained using LCOGTN telescopes, and data gathered from ASAS-3, ASAS-SN, TESS, and GDS projects spanning a period of about 18 years. Radial velocities were determined using spectroscopic observations obtained at LCO/duPont and ESO-LSO/2p2 telescopes in the framework of "OWN Survey" and "B-SUGOS" projects.</p>
Eclipsing binary systems with beta Cephei components. V1216 Sco
<p>A set of files for MESA 23.05.1 and GYRE 7.1, used to compute a grid of binary evolutionary tracks and stellar oscillation models used in the paper "Eclipsing binary systems with beta Cephei components. V1216 Sco".</p>
A window into δ Sct stellar interiors: understanding the eclipsing binary system TT Hor
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.480.1372S/abstract">A window into δ Sct stellar interiors: understanding the eclipsing binary system TT Hor</a></p>
Tidally Induced Pulsations in Kepler Eclipsing Binary KIC 3230227
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017ApJ...834...59G">Guo et al. (2017)</a>. MESA version 8118.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-4357/834/1/59">10.3847/1538-4357/834/1/59</a></p>
Modelling Kepler red giants in eclipsing binaries: calibrating the mixing-length parameter with asteroseismology
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.475..981L/abstract">Li et al. (2018)</a>. MESA version 8118.</p> <p>Publication DOI: <a href="https://doi.org/10.1093/mnras/stx3079">10.1093/mnras/stx3079</a></p>
A Photometric, Spectroscopic, and Apsidal Motion Analysis of the F-type Eclipsing Binary BW Aquarii from K2 Campaign 3
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018AJ....156....8L/abstract">Lester & Gies (2018)</a>. MESA version 10108.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-3881/aac2ea">10.3847/1538-3881/aac2ea</a> </p>
Age determination of galactic B-type stars in double-lined eclipsing binaries
<p>We present the results of age determination for galactic B-type main sequence stars which are components of double-lined eclipsing binaries. Only detached systems are considered. We analyze 38 binary systems that meet such criteria. The analysis is based on evolutionary computations and we consider that the age is determined if there is a common value from the radius−age diagrams and the agreement in the position of both components in the Hertzsprung-Russell diagram. In some cases, to meet these two conditions, it was necessary to adjust the value of the metallicity, Z or/and the parameter of overshooting from the convective core, αov. We determine the consistent age for 33 binaries out of 38. Besides, we made an extensive computations and for each system we give the range of αov and Z, for which the consistent solutions exist. The age of the studied B-type main sequence stars ranges, as counted from the Zero Age Main Sequence, from about 2.5 Myr to about 200 Myr.</p>
Tidally perturbed g-mode pulsations in a sample of close eclipsing binaries
<p>Description:<br> Reduced Kepler and TESS light curves of KIC 3228863, KIC 3341457, KIC 4947528, KIC 9108579, and<br> KIC 12785282, as well as various data products obtained at different steps of the analysis presented in Van Reeth<br> et al. (2023): the residual pulsation light curves (after subtracting the harmonic model for the binarity), the<br> optimised prewhitened (Kepler) frequency lists, measured g-mode patterns, and detected tidal g-mode<br> perturbations (both measured directly from orbital-phase-binned data and reconstructed using detected<br> orbital-frequency-spaced multiplets).</p> <p>Abstract:<br> Context. Thanks to the high-precision photometry from space missions such as Kepler and TESS, tidal<br> perturbations and tilting of pulsations have been detected in more than a dozen binary systems. However, only<br> two of these were gravity-mode (g-mode) pulsators.<br> Aims. We aim to detect tidally perturbed g modes in additional binary systems and characterise them<br> observationally.<br> Methods. We perform a custom data reduction of the available Kepler and TESS photometry of a well-studied,<br> published sample of 35 binary systems with gamma Doradus (gamma Dor) pulsators. For each target, we model<br> the binary signal using a sum of 100 sine waves, with frequencies at orbital harmonics, and measure significant<br> pulsation frequencies in an iterative prewhitening analysis of the residual light curve. Pulsations are<br> labelled as tidally perturbed g modes if they are part of both period-spacing patterns and multiplets spaced by<br> integer multiples of the orbital frequency. After visual inspection and confirmation, the properties of these<br> targets and g modes are characterised.<br> Results. We detect tidally perturbed g-mode pulsations for five short-period binaries that are circularised and<br> (almost) synchronously rotating: KIC 3228863, KIC 3341457, KIC 4947528, KIC 9108579, and KIC 12785282.<br> Tidally perturbed g modes that occur within the same star and have the same mode identification (k,m), are found<br> to have near-identical relative amplitude and phase modulations, which are within their respective 1-sigma<br> uncertainties also identical for the Kepler and TESS photometric passbands. By contrast, pulsations with<br> different mode identification (k,m) are found to exhibit different modulations. Moreover, the observed<br> amplitude and phase modulations are correlated, indicating that the binary tides primarily distort the g-mode<br> amplitudes on the stellar surface. The phase modulations are then primarily a geometric effect of the<br> integration of the stellar flux over the visible stellar surface. All selected binaries also exhibit signal<br> that resembles rotational modulation in the Fourier domain. In the case of KIC 3228863, this is caused by the<br> presence of the known tertiary component, and for the other systems we hypothesise that it is caused by<br> temperature variations on the stellar surface. Alternatively, the signal can be overstable convective modes in<br> the stellar core or belong to the non-pulsating companion.<br> Conclusions. While g-mode pulsation periods are known to be a direct probe of the deep interior stellar<br> structure, the binary tides which cause the pulsation modulations are dominant in the outer stellar layers.<br> Hence, in future tidally perturbed g modes may allow us to do core-to-surface asteroseismic modelling of<br> tidally distorted stars.</p>
First photometric study and Light curve analysis of the four short period eclipsing binaries: $ZTFJ000030.44 +391106.9$, $ZTFJ000817.08+402532.1$, $ZTFJ002158.44+252934.04$ and $ZTFJ003357.62+415747.8$
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Table A.5: Eclipsing binaries
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The eclipsing binary systems with delta Scuti component. AB Cas
<p>A set of inlists for MESA v12115, used to compute a grid of binary evolutionary tracks used in the paper "The eclipsing binary systems with delta Scuti component. AB Cas".</p>
Differential Rotation in Convective Envelopes: Constraints from Eclipsing Binaries
<p>Data, inlists, and scripts associated with doi:10.1093/mnras/stz2983</p>
Results of Modeling Kepler Eclipsing Binaries: Homogeneous Inference of Orbital & Stellar Properties
<p>These are the parameter estimation results (thinned versions of the full MCMC analysis) from the paper "Modeling Kepler Eclipsing Binaries: Homogeneous Inference of Orbital & Stellar Properties" by Windemuth et al. (2019). </p>
RASS/All-Sky Automated Survey Eclipsing Binaries Catalog
The authors have combined their catalog of eclipsing binaries from the All-Sky Automated Survey (ASAS) with the ROSAT All-Sky Survey (RASS) Bright and Faint Source Catalogs (RASSBSC and RASSFSC). The combination using a matching radius of 50 arcseconds results in 836 eclipsing binaries that display coronal activity and is the largest sample of active binary stars assembled to the date of publication. By using the (V-I) colors of the ASAS eclipsing binary catalog, the authors are able to determine the distances and thus bolometric luminosities for the majority of eclipsing binaries that display significant stellar activity. A typical value for the ratio of soft X-ray to bolometric luminosity is L<sub>X</sub>/L<sub>bol</sub> ~ a few x 10<sup>-4</sup>, similar to the ratio of soft X-ray to bolometric flux F<sub>X</sub>/F<sub>bol</sub> in the most active regions of the Sun. Unlike rapidly rotating isolated late-type dwarfs - stars with significant outer convection zones - a tight correlation between Rossby number and activity of eclipsing binaries is absent. The authors find evidence for the saturation effect and marginal evidence for the so-called "super-saturation" phenomena. Their work shows that wide-field stellar variability searches can produce a high yield of binary stars with strong coronal activity. The authors expect that only 1.4% (i.e., 12 out of 836) of the matches between the ASAS eclipsing binary and RASS sources will be false given their maximum angular separation criterion of 50 arcseconds. This Browse table excludes 29 contact binaries for which the separate distance estimates made by the authors using the source V-band and I-band magnitudes differed by more than 20%, and hence contains 807 (836 - 29) eclipsing and X-ray emitting binary systems. Complete information on ASAS and its freely accessible data are available at the ASAS web site: <a href="http://www.astrouw.edu.pl/asas/">http://www.astrouw.edu.pl/asas/</a>. This table was created by the HEASARC in July 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/AcA/58/405">CDS catalog J/AcA/58/405</a> file catalog.dat. This is a service provided by NASA HEASARC .
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