J/ApJS/276/17 Short-period heartbeat binaries from TESS (Solanki+, 2025)
Short-period heartbeat binaries from TESS Full-Frame Images.
Solanki S., Cieplak A.M., Schnittman J., Baker J.G., Barclay T.,
Barry R.K., Kostov V., Kruse E., Olmschenk G., Powell B.P.,
Ishitani Silva S., Torres G.
<Astrophys. J. Suppl. Ser., 276, 17 (2025)>
=2025ApJS..276...17S 2025ApJS..276...17S
ADC_Keywords: Binaries, eclipsing; Magnitudes, absolute; Stars, masses;
Photometry
Keywords: Eclipsing binary stars ; Close binary stars
Abstract:
We identify 240 short-period (P≲10 days) binary systems in Transiting
Exoplanet Survey Satellite data, 180 of which are heartbeat binaries.
The sample is mostly a mix of A- and B-type stars and primarily
includes eclipsing systems, where over 30% of the sources with primary
and secondary eclipses show a secular change in their intereclipse
timings and relative eclipse depths over a multiyear timescale, likely
due to orbital precession. The orbital parameters of the population
are estimated by fitting a heartbeat model to their phase curves and
Gaia magnitudes, where the model accounts for ellipsoidal variability,
Doppler beaming, reflection effects, and eclipses. We construct the
sample's period-eccentricity distribution and find an eccentricity
cutoff (where e->0) at a period of 1.7 days. Additionally, we measure
the periastron advance rate for 12 of the precessing sources and find
that they all exhibit prograde apsidal precession, which is as high as
9°/yr for one of the systems. Using the inferred stellar
parameters, we estimate the general relativistic precession rate of
the argument of periastron for the population and expect over
30 systems to show a precession in excess of 0.3°/yr.
Description:
An initial list of 240 heartbeat candidates was constructed using two
convolutional neural networks (CNNs) that independently looked through
the light curves generated from the Transiting Exoplanet Survey
Satellite (TESS; launched April 18, 2018) Full-Frame Images (FFIs).
After identifying the candidate heartbeats (see Section 2), light
curves up through TESS Sector 67 (2023-Jul-29) were generated. Light
curves from Sectors 1-26 have a 30min cadence, those from Sectors
27-55 have a 10min cadence, and ones from Sectors 56-67 have a 200s
cadence.
The final light-curve sample of 180 heartbeats contains 133 eclipsing
systems, of which 36 systems show a single eclipse and 97 show two
eclipses per orbit.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 137 180 The Gaia magnitudes, periods, and other inferred
parameters from the MCMC fits to the phase curves
of the 180 heartbeat candidates
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See also:
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
I/357 : Gaia DR3 Part 3. Non-single stars (Gaia Collaboration, 2022)
J/A+A/450/681 : Companions to close spectroscopic binaries (Tokovinin+, 2006)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
J/MNRAS/455/4136 : Kepler triples (Borkovits+, 2016)
J/AJ/151/68 : Kepler Mission. VII. Eclipsing binaries in DR3 (Kirk+, 2016)
J/ApJ/829/34 : Kepler heartbeat star radial velocities (Shporer+, 2016)
J/MNRAS/467/1830 : Starspots on A stars (Balona, 2017)
J/AJ/157/196 : Close companions around young stars (Kounkel+, 2019)
J/A+A/641/A157 : Limb-darkening coefficients for white dwarfs (Claret+, 2020)
J/AJ/161/273 : 181 new planet candidates with TESS (Olmschenk+, 2021)
J/ApJS/259/66 : Eclipsing quadruple star candidates from TESS (Kostov+, 2022)
J/ApJS/258/16 : TESS Eclipsing Binary stars. I. Sectors 1-26 (Prsa+, 2022)
J/ApJS/259/16 : Heartbeat stars in Gal. bulge & MCs from OGLE (Wrona+, 2022)
J/A+A/683/A158 : Six new triple stellar systems time of minima (Zasche+, 2024)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 I10 --- TIC [8772474/2046878952] TIC identifier
12- 16 F5.2 mag GMag [-7.3/4.9] Absolute Gaia DR3 G-band magnitude
18- 21 F4.2 mag e_GMag [0.05/7.8] GMag uncertainty
23- 30 F8.5 d Per [1.47/17.8] Period
32- 38 F7.5 d e_Per [2e-05/0.01] Per uncertainty
40- 43 F4.1 Msun M1 [0.6/92] Primary stellar mass
45- 48 F4.1 Msun e_M1 [0/11.3] Lower uncertainty on M1
50- 53 F4.1 Msun E_M1 [0.1/88] Upper uncertainty on M1
55- 58 F4.1 Msun M2 [0.1/22] Secondary stellar mass
60- 62 F3.1 Msun e_M2 [0/3.7] Lower uncertainty on M2
64- 67 F4.1 Msun E_M2 [0/33] Upper uncertainty on M2
69- 73 F5.3 --- e [0.2/0.8] Eccentricity
75- 79 F5.3 --- e_e [0/0.1] Lower uncertainty on e
81- 85 F5.3 --- E_e [0/0.25] Upper uncertainty on e
87- 91 F5.2 deg inc [20.3/89.6] Inclination
93- 97 F5.2 deg e_inc [0.09/33.2] Lower uncertainty on inc
99- 103 F5.2 deg E_inc [0.13/34.6] Upper uncertainty on inc
105- 110 F6.2 deg omega [-79.2/76.2] Argument of periastron, ω
112- 116 F5.2 deg e_omega [0.25/36.5] Lower uncertainty on omega
118- 122 F5.2 deg E_omega [0.22/74.6] Upper uncertainty on omega
124- 127 F4.2 --- Blend [0.04/0.84] Blending
129- 132 F4.2 --- e_Blend [0.01/0.3] Lower uncertainty on Blend
134- 137 F4.2 --- E_Blend [0.01/0.41] Upper uncertainty on Blend
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 27-Oct-2025