TESS Eclipsing Binary Stars. I. Short cadence observations of 4584 eclipsing binaries in Sectors 1-26

Prsa, Andrej; Kochoska, Angela; Conroy, Kyle E.; Eisner, Nora; Hey, Daniel R.; IJspeert, Luc; Kruse, Ethan; Fleming, Scott W.; Johnston, Cole; Kristiansen, Martti H.; LaCourse, Daryll; Mortensen, Danielle; Pepper, Joshua; Stassun, Keivan G.; Torres, Guillermo; Abdul-Masih, Michael; Chakraborty, Joheen; Gagliano, Robert; Guo, Zhao; Hambleton, Kelly; Hong, Kyeongsoo; Jacobs, Thomas; Jones, David; Kostov, Veselin; Lee, Jae Woo; Omohundro, Mark; Orosz, Jerome A.; Page, Emma J.; Powell, Brian P.; Rappaport, Saul; Reed, Phill; Schnittman, Jeremy; Schwengeler, Hans Martin; Shporer, Avi; Terentev, Ivan A.; Vanderburg, Andrew; Welsh, William F.; Caldwell, Douglas A.; Doty, John P.; Jenkins, Jon M.; Latham, David W.; Ricker, George R.; Seager, Sara; Schlieder, Joshua E.; Shiao, Bernie; Vanderspek, Roland; Winn, Joshua N.

doi:10.48550/arxiv.2110.13382

Cited by 5 publications

(5 citation statements)

References 75 publications

(83 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Tight binary systems are those whose orbits are sufficiently close to significantly tidally distort the star and cause measurable variation in the light curve (see for example Ko laczek-Szymański et al 2021;Prsa et al 2021)and occasionally are even aligned such that one star eclipses the other. Observations are limited to very small orbits and short periods ( 1 month).…”

Section: A Brief Comparison Of Methods For Binary Identificationmentioning

confidence: 99%

Astrometric Identification of Nearby Binary Stars I: Predicted Astrometric Signals

Penoyre,

Belokurov,

Evans

2021

Preprint

View full text Add to dashboard Cite

We examine the capacity to identify binary systems from astrometric deviations alone. We generate a broad catalog of simulated binary systems within 100 pc, and examine synthetic observations matching the Gaia survey's scanning law and astrometric data processing routine. We show how the Unit Weight Error (UWE) and Proper Motion Anomaly (PMA) vary as a function of period, and the properties of the binary. Both UWE and PMA peak for systems with a binary period close to the time baseline of the survey. Thus UWE can be expected to increase or remain roughly constant as we observe the same system over a longer baseline, and we suggest UW E eDR3 > 1.25 and ∆UW E/UW E eDR3 > −0.25 as criteria to select astrometric binaries whilst excluding other sources of astrometric noise. We show that for stellar binaries we would expect to detect significant astrometric deviations for 80-90% of our simulated systems with periods ranging from months to decades. We confirm that for systems with periods less than the survey's baseline the observed UW E scales ∝ ϖ (parallax), a (semi-major axis) and ∆ = |q−l| (1+q)(1+l) where q and l are the mass and light ratio respectively, with a modest dependence on viewing angle. We show that for longer periods the signal is suppressed by a factor of roughly ∝ P −2 (period). PMA is largest in orbits with slightly longer periods but obeys the same approximate scaling relationships. We are able to predict the distribution of multiple observable astrometric indicators and show that binary systems in the above period range will be distinct and differentiable from single stars.

show abstract

Section: A Brief Comparison Of Methods For Binary Identificationmentioning

confidence: 99%

Astrometric Identification of Nearby Binary Stars I: Predicted Astrometric Signals

Penoyre,

Belokurov,

Evans

2021

Preprint

View full text Add to dashboard Cite

show abstract

“…From a vast number of known eclipsing binary systems (e.g., Prša et al 2011;LaCourse et al 2015;Kirk et al 2016;Prsa et al 2021) there are only a few well-studied close binaries that contain 𝛿 Sct components, e.g., TT Hor (Streamer et al 2018) and KIC 10661783 (Miszuda et al 2021). These systems, thanks to the detailed evolutionary modelling, have precise estimates of the initial parameters that allow to reconstruct their evolution.…”

Section: Binary-evolution Modelsmentioning

confidence: 99%

The eclipsing binary systems with $δ$ Scuti component -- II. AB Cas

Miszuda,

Kołaczek-Szymański,

Szewczuk

et al. 2022

Preprint

View full text Add to dashboard Cite

We present a complex study of the eclipsing binary system, AB Cas. The analysis of the whole TESS light curve, corrected for the binary effects, reveals 112 significant frequency peaks with 17 independent signals. The dominant frequency 𝑓 1 = 17.1564 d −1 is a radial fundamental mode. The 𝑂 − 𝐶 analysis of the times of light minima from over 92 years leads to a conclusion that due to the ongoing mass transfer the system exhibits a change of the orbital period at a rate of 0.03 s per year. In order to find evolutionary models describing the current stage of AB Cas, we perform binary evolution computations. Our results show the AB Cas system as a product of the rapid non-conservative mass transfer with about 5-26% of transferred mass lost from the system. This process heavily affected the orbital characteristics of this binary and its components in the past. In fact, this system closely resemble the formation scenarios of EL CVn type binaries. For the first time, we demonstrate the effect of binary evolution on radial pulsations and determine the lines of constant frequency on the HR diagram. From the binary and seismic modelling, we obtain constraints on various parameters. In particular, we constrain the overshooting parameter, 𝑓 ov ∈ [0.010, 0.018], the mixing-length parameter, 𝛼 MLT ∈ [1.2, 1.5] and the age, 𝑡 ∈ [2.3, 3.4] Gyr.

show abstract

“…Another highlight from Kepler and TESS is the discovery and characterization of heartbeat stars, triggering the beginnings of tidal asteroseismology (e.g., Hambleton et al 2013;Bowman et al 2019;Handler et al 2020). Thus far, about 180 heartbeat stars have been identified in the entire Kepler data (Kirk et al 2016), and Prsa et al (2021) discovered 22 heartbeat binaries in the 2 minute TESS data up to Sector 26, but a handful of them have been closely studied.…”

Section: Introductionmentioning

confidence: 99%

FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations

Wang

Ren

Andersen

et al. 2023

View full text Add to dashboard Cite

We present a detailed analysis of an eclipsing double-lined binary FX UMa based on TESS photometry and newly acquired spectroscopic observations. The radial velocities and atmospheric parameters for each component star are obtained from the SONG high-resolution spectra. Combined with the radial-velocity measurements, our light-curve modeling yields absolute masses and radii of the two components. The Fourier amplitude spectrum of the residual light curve reveals a total of 103 frequencies with signal-to-noise ratio (S/N) ≥ 4, including 12 independent frequencies, 17 multiples of the orbital frequency (Nf orb), and 74 combination frequencies. Ten Nf orb peaks with S/N > 10 have very high amplitudes and are likely due to tidally excited oscillations (TEOs). The remaining Nf orb peaks (4 ≤ S/N ≤ 10) may be originated from the imperfect removal, or they are actually real TEOs. Four anharmonic frequencies can pair up and sum to give exact harmonics of the orbital frequency, suggesting the existence of nonlinear tidal processes in the eccentric binary system FX UMa. Eight independent frequencies in the range of 20–32 day−1 are typical low-order pressure modes of δ Scuti pulsators.

show abstract

TESS Eclipsing Binary Stars. I. Short cadence observations of 4584 eclipsing binaries in Sectors 1-26

Cited by 5 publications

References 75 publications

Astrometric Identification of Nearby Binary Stars I: Predicted Astrometric Signals

Astrometric Identification of Nearby Binary Stars I: Predicted Astrometric Signals

The eclipsing binary systems with $δ$ Scuti component -- II. AB Cas

FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations

Contact Info

Product

Resources

About