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arxiv: 2605.20080 · v1 · pith:IGTYMJEEnew · submitted 2026-05-19 · 🌌 astro-ph.SR

TIC 295741342: A Triply-Eclipsing Triple Star System with a Giant Tertiary

Brian P. Powell , Guillermo Torres , Veselin B. Kostov , Saul A. Rappaport , Tam\'as Borkovits , Robert Gagliano , David W. Latham This is my paper

Pith reviewed 2026-05-20 03:48 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords triply-eclipsing triplegiant tertiaryRoche lobe overflowTESS photometryspectro-photodynamical modeleclipsing binarystellar evolutioncoplanar orbits
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The pith

A triply-eclipsing triple star system contains a giant tertiary that will overflow its Roche lobe in either of two evolutionary states.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents the discovery and full characterization of TIC 295741342, a system in which two main-sequence stars in a 4.75-day eclipsing binary orbit a giant tertiary star every 412.8 days. Analysis of TESS photometry, radial velocities, and spectral energy distribution yields two degenerate solutions for the giant: one ascending the red giant branch and one on the horizontal branch heading toward the asymptotic giant branch. Both solutions indicate near-perfect coplanarity of the orbits. A distinctive head-and-shoulders eclipse directly measures the relative sizes and light contributions of all three stars. The models predict that the tertiary will fill its Roche lobe and initiate mass transfer or common-envelope evolution.

Core claim

TIC 295741342 consists of an inner eclipsing binary with a 4.75-day period and an outer 412.8-day orbit around a giant tertiary star. Two solutions are found for the tertiary's state, both with near-perfect coplanarity, and both predict future Roche-lobe overflow that will produce either stable mass transfer or common-envelope evolution. Comprehensive spectro-photodynamical modeling of the TESS light curve, eclipse timings, 48 radial-velocity spectra, and spectral energy distribution fixes the stellar radii, masses, and temperatures while the head-and-shoulders eclipse in Sector 33 supplies direct flux and radius ratios.

What carries the argument

A spectro-photodynamical model that simultaneously fits the TESS light curve, eclipse times, spectral energy distribution, and radial velocities from 48 spectra, combined with MIST evolutionary tracks to place the giant tertiary on either the red giant branch or horizontal branch.

If this is right

  • The giant tertiary will overflow its Roche lobe while ascending the red giant branch in one solution or the asymptotic giant branch in the other.
  • Roche-lobe overflow will initiate either stable mass transfer onto the inner binary or common-envelope evolution that may produce ejections or mergers.
  • The midpoint of the next outer eclipse is predicted to occur on September 1 2026, providing an immediate observational test.
  • Continued monitoring of eclipse timings will further constrain the orbital elements and distinguish the two solutions.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Detection of the predicted outer eclipse would also test whether the inner binary survives the mass-transfer phase intact.
  • The near-coplanarity may indicate formation through disk fragmentation or later dynamical alignment, offering a benchmark for triple-star formation models.
  • Systems like this could be used to calibrate the onset of common-envelope evolution when a giant overflows onto a close binary.

Load-bearing premise

The MIST evolutionary tracks correctly identify the current state of the giant tertiary and its future Roche-lobe overflow behavior in both the red-giant-branch and horizontal-branch solutions.

What would settle it

Precise photometry of the outer eclipse near September 1 2026 that either matches the predicted midpoint and depth or deviates enough to rule out one or both evolutionary states.

Figures

Figures reproduced from arXiv: 2605.20080 by Brian P. Powell, David W. Latham, Guillermo Torres, Robert Gagliano, Saul A. Rappaport, Tam\'as Borkovits, Veselin B. Kostov.

Figure 1
Figure 1. Figure 1: TIC 295741342 outer-body eclipse. The TESS flux is shown in black points, with horizontal dashed red lines indicating the depths of the ‘shoulders’ and ‘head’ of the outer body eclipse, which substantially constrains the relative fluxes of the stars in the system in the TESS band. the flat “shoulders” of the eclipse, and another horizon￾tal red line at 5% corresponding to the depth of the “head.” The shape… view at source ↗
Figure 2
Figure 2. Figure 2: TESS Full-Frame Image QLP lightcurves (black) for TIC 295741342 from Sectors 7 (upper left), 33 (upper right), 34 (lower left), and 87 (lower right), plotted against the RGB-s model fit (solid red line) and the HB-s model fit (dashed blue line) – the two fits are nearly identical so they are overlapping in the plot. Differences can be seen in the residuals. Residuals are shown in panels below each sector f… view at source ↗
Figure 3
Figure 3. Figure 3: TRES RV measurements (points) and model RVs (lines) for stars Aa (red), Ab (blue), and B (green) for the duration of the model simulation (top left) and at time segments BJD 2459502 - 2459697 (top right), BJD 2459925 - 2460067 (middle left), BJD 2460278 - 2460427 (middle right), BJD 2460598 - 2460717 (bottom left), and BJD 2460960 - 2461060 (bottom right). Each of the five panels (after the first panel) re… view at source ↗
Figure 4
Figure 4. Figure 4: ETV curves for RGB-s (top panel) and HB-s (bottom panel) from BJD 2458466.00 to 2460747.00 with primary measured ETVs (red circles), secondary measured ETVs (blue circles), primary model curve (red line), and secondary model curve (blue line). dashed blue line with the 1σ and 2σ bands in shades of blue created in the same manner. A gray vertical line indicates the time of the minimum distance between the t… view at source ↗
Figure 5
Figure 5. Figure 5: TIC 295741342 model SED fit at the star for RG￾B-s (top panel) and HB-s (bottom panel). The model curves in both panels are nearly identical. The binary components Aa and Ab are shown in blue and green, respectively. The tertiary is shown in orange, with the total SED in black. The total and the tertiary overlap in both solutions as the SED is dominated by the giant. of the evolution of the radii in the le… view at source ↗
Figure 6
Figure 6. Figure 6: A detailed view of the HB solution outer eclipse event over nine timesteps. (upper panels) View from the negative Z direction of stars Aa (red), Ab (blue), and B (green). When stars Aa and Ab pass behind B, we show their positions as dashed outlines for clarity. (lower panels) TESS lightcurve data (black dots) for the duration of the outer eclipse event. The dashed vertical red line shows the time correspo… view at source ↗
Figure 7
Figure 7. Figure 7: Lightcurves of outer eclipses for the duration of the model fit and future projections. The best model flux is shown as a red line, with 1σ and 2σ uncertainty bands created from 1,000 random parameter sets in the posterior. The vertical gray line is the time of the closest approach between the tertiary and the center of mass of the binary in the XY-plane with 1σ and 2σ bands. The title of each panel gives … view at source ↗
Figure 8
Figure 8. Figure 8: (left panels) Visualizations of the radii of the stars in TIC 295741342 as the system evolves. For RGB-s in the top row, the radii of stars Aa and Ab will slightly decrease over the duration in both cases. The radius of star B (green) will grow rapidly as it ascends the RGB. In 54 Myr, star B will overflow its Roche lobe with a radius of 83 R⊙. For HB-s in the bottom row, the system has survived star B’s f… view at source ↗
Figure 9
Figure 9. Figure 9: (left panel) Histogram of 105 dwell times calculated in the process described in Section 6.4 with parameter sets randomly sampled from the posteriors RGB-s (red) and HB-s (blue). Median dwell times and the 1σ range are noted for both solutions in the upper right, with median values shown as dashed vertical lines. (right panel) CDF of the HB/RGB dwell time ratio calculated from the same samples. The median … view at source ↗
read the original abstract

We present the discovery and characterization of TIC 295741342, a triply-eclipsing triple star system with a giant tertiary. The eclipsing binary consists of two similar main-sequence stars in a 4.75-day orbit. The binary is in a 412.8-day orbit with the giant tertiary. We found two degenerate solutions for the system: one where the tertiary is ascending the Red Giant Branch (RGB), and the other where the tertiary is on the Horizontal Branch (HB) and will eventually ascend the Asymptotic Giant Branch (AGB). In both solutions, the system is near-perfectly coplanar. In TESS Sector 33, the binary passes behind the giant tertiary, producing a distinctive "head-and-shoulders" eclipse that directly constrains the relative flux contributions and radii of all three stars. We modeled the system using a comprehensive spectro-photodynamical model that simultaneously fits the TESS lightcurve, eclipse times, spectral energy distribution, and radial velocities from 48 TRES spectra obtained over four years of observation resolving all three components. Evolutionary analysis using MIST tracks indicates that, in both solutions, the tertiary will overflow its Roche lobe, one in the RGB and the other in the AGB. The Roche lobe overflow will initiate either a stable mass transfer to the binary or a common envelope evolution that will likely result in ejections and/or mergers. Our models predict the midpoint of the next outer eclipse will occur on September 1, 2026 and we encourage follow-up observations with a $\pm$3 day window to observe the full event and further constrain the system parameters.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. The manuscript presents the discovery and characterization of TIC 295741342, a triply-eclipsing triple star system consisting of a 4.75-day eclipsing binary of two similar main-sequence stars in a 412.8-day orbit with a giant tertiary. A joint spectro-photodynamical model is used to fit the TESS light curve (including a distinctive head-and-shoulders eclipse in Sector 33), eclipse times, spectral energy distribution, and 48 TRES radial velocities resolving all three components. Two degenerate solutions are reported for the tertiary: ascending the red giant branch or on the horizontal branch en route to the asymptotic giant branch. Both solutions are near-perfectly coplanar. MIST evolutionary tracks indicate future Roche-lobe overflow (RGB or AGB phase) that may lead to stable mass transfer or common-envelope evolution, with a predicted next outer eclipse midpoint on 1 September 2026.

Significance. If the results hold, the work is significant as a rare, well-constrained example of a hierarchical triple containing a giant tertiary. The head-and-shoulders eclipse and resolved spectra provide direct constraints on relative radii and flux contributions, while the multi-dataset fit (photometry, RVs, SED) strengthens the orbital elements and stellar parameters. The dual evolutionary pathways and explicit prediction for follow-up observations are of interest for studies of triple-star dynamics and future binary evolution involving mass transfer or mergers.

major comments (1)
  1. [evolutionary analysis paragraph] Evolutionary analysis paragraph: the manuscript reports two degenerate solutions for the tertiary but does not describe a joint isochrone fit or explicit test that the derived tertiary mass, radius, and Teff are consistent with the same age as the main-sequence lifetime of the inner 4.75-day binary. MIST assumptions on overshooting, mass loss, and metallicity could shift the track classification, affecting the viability of both solutions and the predicted Roche-lobe overflow behavior.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and positive assessment of the manuscript's significance. We address the single major comment below regarding the evolutionary analysis.

read point-by-point responses

  1. Referee: Evolutionary analysis paragraph: the manuscript reports two degenerate solutions for the tertiary but does not describe a joint isochrone fit or explicit test that the derived tertiary mass, radius, and Teff are consistent with the same age as the main-sequence lifetime of the inner 4.75-day binary. MIST assumptions on overshooting, mass loss, and metallicity could shift the track classification, affecting the viability of both solutions and the predicted Roche-lobe overflow behavior.

    Authors: We thank the referee for this observation. The inner binary components are main-sequence stars whose main-sequence lifetime (several Gyr for ~1.2 solar-mass stars) provides only a broad upper limit rather than a tight age constraint. The tertiary parameters were obtained from the joint spectro-photodynamical fit and then placed on MIST tracks independently to identify the two degenerate solutions. We agree that an explicit discussion of age consistency and sensitivity to MIST parameters would strengthen the section. In the revised manuscript we will add a paragraph that (i) compares the implied system age from the tertiary tracks to the inner binary's main-sequence lifetime under standard MIST assumptions, (ii) notes that both the RGB and HB solutions remain consistent within the derived uncertainties, and (iii) briefly explores the effects of varying overshooting, mass-loss rates, and metallicity on the track classification and Roche-lobe overflow predictions. These additions will be included without altering the core results. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper derives its results through direct fitting of orbital elements, stellar parameters, and relative fluxes to observational data (TESS light curve, eclipse times, SED, and 48 TRES RVs) via a spectro-photodynamical model. The two degenerate solutions for the tertiary (RGB vs. HB) are obtained by applying external MIST evolutionary tracks to the fitted mass, radius, and Teff values; this is an interpretive step using independent stellar models rather than a reduction of the claim to the inputs by construction. The predicted next outer eclipse midpoint follows from forward integration of the fitted 412.8-day outer orbit and is a standard extrapolation, not a relabeling of a fitted quantity. No self-definitional relations, fitted inputs presented as predictions, load-bearing self-citations, or ansatz smuggling appear in the chain. The analysis remains self-contained against the external data and models.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The claim rests on standard stellar evolution tracks and fitted parameters from observational data; no new physical entities are introduced.

free parameters (2)
  • orbital periods, inclinations, and stellar radii
    Fitted simultaneously to TESS light curve, eclipse timings, and radial velocities
  • relative flux contributions
    Constrained by the head-and-shoulders eclipse morphology in Sector 33
axioms (1)
  • domain assumption MIST evolutionary tracks correctly map the tertiary's current state and future Roche-lobe overflow timing
    Invoked to classify the two degenerate solutions and predict mass transfer

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Works this paper leans on

76 extracted references · 76 canonical work pages · 6 internal anchors

  1. [1]

    2015, TensorFlow: Large-Scale Machine Learning on Heterogeneous Systems, https://www.tensorflow.org/

    Abadi, M., Agarwal, A., Barham, P., et al. 2015, TensorFlow: Large-Scale Machine Learning on Heterogeneous Systems, https://www.tensorflow.org/

    work page 2015

  2. [2]

    2014, in IAU Symposium, Vol

    Allard, F. 2014, in IAU Symposium, Vol. 299, Exploring the Formation and Evolution of Planetary Systems, ed. M. Booth, B. C. Matthews, & J. R. Graham, 271–272, doi: 10.1017/S1743921313008545

    work page doi:10.1017/s1743921313008545 2014

  3. [3]

    J., Hoyer, S., et al

    Alonso, R., Deeg, H. J., Hoyer, S., et al. 2015, A&A, 584, L8, doi: 10.1051/0004-6361/201527109 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f

    work page doi:10.1051/0004-6361/201527109 2015

  4. [4]

    2024, A&A, 692, A247, doi: 10.1051/0004-6361/202452637

    Bashi, D., & Tokovinin, A. 2024, A&A, 692, A247, doi: 10.1051/0004-6361/202452637

    work page doi:10.1051/0004-6361/202452637 2024

  5. [5]

    2016, MNRAS, 455, 4136, doi: 10.1093/mnras/stv2530

    Borkovits, T., Hajdu, T., Sztakovics, J., et al. 2016, MNRAS, 455, 4136, doi: 10.1093/mnras/stv2530

    work page doi:10.1093/mnras/stv2530 2016

  6. [6]

    2015, MNRAS, 448, 946, doi: 10.1093/mnras/stv015

    Borkovits, T., Rappaport, S., Hajdu, T., & Sztakovics, J. 2015, MNRAS, 448, 946, doi: 10.1093/mnras/stv015

    work page doi:10.1093/mnras/stv015 2015

  7. [7]

    A., Hajdu, T., et al

    Borkovits, T., Rappaport, S. A., Hajdu, T., et al. 2020a, MNRAS, 493, 5005, doi: 10.1093/mnras/staa495

    work page doi:10.1093/mnras/staa495

  8. [8]

    A., Toonen, S., et al

    Borkovits, T., Rappaport, S. A., Toonen, S., et al. 2022a, MNRAS, 515, 3773, doi: 10.1093/mnras/stac1983

    work page doi:10.1093/mnras/stac1983

  9. [9]

    2019, MNRAS, 483, 1934, doi: 10.1093/mnras/sty3157

    Borkovits, T., Rappaport, S., Kaye, T., et al. 2019, MNRAS, 483, 1934, doi: 10.1093/mnras/sty3157

    work page doi:10.1093/mnras/sty3157 2019

  10. [10]

    A., Tan, T

    Borkovits, T., Rappaport, S. A., Tan, T. G., et al. 2020b, MNRAS, 496, 4624, doi: 10.1093/mnras/staa1817

    work page doi:10.1093/mnras/staa1817

  11. [11]

    A., et al

    Borkovits, T., Mitnyan, T., Rappaport, S. A., et al. 2022b, MNRAS, 510, 1352, doi: 10.1093/mnras/stab3397

    work page doi:10.1093/mnras/stab3397

  12. [12]

    A., Mitnyan, T., et al

    Borkovits, T., Rappaport, S. A., Mitnyan, T., et al. 2025a, A&A, 695, A209, doi: 10.1051/0004-6361/202453616

    work page doi:10.1051/0004-6361/202453616

  13. [13]

    A., Mitnyan, T., et al

    Borkovits, T., Rappaport, S. A., Mitnyan, T., et al. 2025b, A&A, 703, A153, doi: 10.1051/0004-6361/202556942

    work page doi:10.1051/0004-6361/202556942

  14. [14]

    J., Koch, D., Basri, G., et al

    Borucki, W. J., Koch, D., Basri, G., et al. 2010, Science, 327, 977, doi: 10.1126/science.1185402 21

    work page doi:10.1126/science.1185402 2010

  15. [15]

    A., Latham, D

    Buchhave, L. A., Latham, D. W., Johansen, A., et al. 2012, Nature, 486, 375, doi: 10.1038/nature11121

    work page doi:10.1038/nature11121 2012

  16. [16]

    A., Bizzarro, M., Latham, D

    Buchhave, L. A., Bizzarro, M., Latham, D. W., et al. 2014, Nature, 509, 593, doi: 10.1038/nature13254

    work page doi:10.1038/nature13254 2014

  17. [17]

    J., Levine, A., Fausnaugh, M., et al

    Burke, C. J., Levine, A., Fausnaugh, M., et al. 2020, TESS-Point: High precision TESS pointing tool,, Astrophysics Source Code Library http://ascl.net/2003.001

    work page 2020

  18. [18]

    , keywords =

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245, doi: 10.1086/167900

    work page doi:10.1086/167900 1989

  19. [19]

    A., Fabrycky, D

    Carter, J. A., Fabrycky, D. C., Ragozzine, D., et al. 2011, Science, 331, 562, doi: 10.1126/science.1201274

    work page doi:10.1126/science.1201274 2011

  20. [20]

    2016 , keywords =

    Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102

    work page internal anchor Pith review doi:10.3847/0004-637x/823/2/102 2016

  21. [21]

    2015, Keras,, https://keras.io

    Chollet, F., et al. 2015, Keras,, https://keras.io

    work page 2015

  22. [22]

    R., Borkovits, T., Mitnyan, T., Rappaport, S

    Czavalinga, D. R., Borkovits, T., Mitnyan, T., Rappaport, S. A., & P´ al, A. 2023a, MNRAS, 526, 2830, doi: 10.1093/mnras/stad2759

    work page doi:10.1093/mnras/stad2759

  23. [23]

    R., Mitnyan, T., Rappaport, S

    Czavalinga, D. R., Mitnyan, T., Rappaport, S. A., et al. 2023b, A&A, 670, A75, doi: 10.1051/0004-6361/202245300

    work page doi:10.1051/0004-6361/202245300

  24. [24]

    MPI for Python: Performance improvements and MPI-2 extensions , journal =

    Dalcin, L., Paz, R., Storti, M., & D’Elia, J. 2008, Journal of Parallel and Distributed Computing, 68, 655, doi: http://dx.doi.org/10.1016/j.jpdc.2007.09.005

    work page doi:10.1016/j.jpdc.2007.09.005 2008

  25. [25]

    L., Borkovits, T., et al

    Derekas, A., Kiss, L. L., Borkovits, T., et al. 2011, Science, 332, 216, doi: 10.1126/science.1201762

    work page doi:10.1126/science.1201762 2011

  26. [26]

    2016 , note =

    Dotter, A. 2016, ApJS, 222, 8, doi: 10.3847/0067-0049/222/1/8

    work page internal anchor Pith review doi:10.3847/0067-0049/222/1/8 2016

  27. [27]

    G., & Struve, O

    Ebbighausen, E. G., & Struve, O. 1956, ApJ, 124, 507, doi: 10.1086/146254

    work page doi:10.1086/146254 1956

  28. [28]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306, doi: 10.1086/670067 Fur´ esz, G. 2008 PhD thesis, Szeged, Hungary Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1, doi: 10.1051/0004-6361/202243940

    work page doi:10.1086/670067 2013

  29. [29]

    Glanz, H., & Perets, H. B. 2021, MNRAS, 500, 1921, doi: 10.1093/mnras/staa3242

    work page doi:10.1093/mnras/staa3242 2021

  30. [30]

    S., Glanz, H., & Neunteufel, P

    Hamers, A. S., Glanz, H., & Neunteufel, P. 2022, ApJS, 259, 25, doi: 10.3847/1538-4365/ac49e7

    work page doi:10.3847/1538-4365/ac49e7 2022

  31. [31]

    R., et al., 2020, @doi [Nature] 10.1038/s41586-020-2649-2 , 585, 357

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2

    work page doi:10.1038/s41586-020-2649-2 2020

  32. [32]

    Research Notes of the American Astronomical Society , keywords =

    Huang, C. X., Vanderburg, A., P´ al, A., et al. 2020a, Research Notes of the American Astronomical Society, 4, 204, doi: 10.3847/2515-5172/abca2e

    work page doi:10.3847/2515-5172/abca2e

  33. [33]

    X., Vanderburg, A., P´ al, A., et al

    Huang, C. X., Vanderburg, A., P´ al, A., et al. 2020b, Research Notes of the American Astronomical Society, 4, 206, doi: 10.3847/2515-5172/abca2d

    work page doi:10.3847/2515-5172/abca2d

  34. [34]

    Hunter, J. D. 2007, Computing in science & engineering, 9, 90

    work page 2007

  35. [35]

    B., Powell, B

    Kostov, V. B., Powell, B. P., Rappaport, S. A., et al. 2022, ApJS, 259, 66, doi: 10.3847/1538-4365/ac5458

    work page doi:10.3847/1538-4365/ac5458 2022

  36. [36]

    B., Rappaport, S

    Kostov, V. B., Rappaport, S. A., Borkovits, T., et al. 2024a, ApJ, 974, 25, doi: 10.3847/1538-4357/ad7368

    work page doi:10.3847/1538-4357/ad7368

  37. [37]

    B., Powell, B

    Kostov, V. B., Powell, B. P., Rappaport, S. A., et al. 2024b, MNRAS, 527, 3995, doi: 10.1093/mnras/stad2947

    work page doi:10.1093/mnras/stad2947

  38. [38]

    B., Powell, B

    Kostov, V. B., Powell, B. P., Fornear, A. U., et al. 2025, ApJS, 279, 50, doi: 10.3847/1538-4365/ade2d8

    work page doi:10.3847/1538-4365/ade2d8 2025

  39. [39]

    B., Powell, B

    Kostov, V. B., Powell, B. P., Rappaport, S. A., et al. 2026, AJ, 171, 29, doi: 10.3847/1538-3881/ae1b8a

    work page doi:10.3847/1538-3881/ae1b8a 2026

  40. [40]

    Shortest period for outer orbit in compact hierarchical triple? Discovery of SB1 around V0885 Per

    Kovalev, M. 2026, arXiv e-prints, arXiv:2604.20314, doi: 10.48550/arXiv.2604.20314

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.20314 2026

  41. [41]

    2016, ARA&A, 54, 271, doi: 10.1146/annurev-astro-081915-023307

    Kratter, K., & Lodato, G. 2016, ARA&A, 54, 271, doi: 10.1146/annurev-astro-081915-023307

    work page doi:10.1146/annurev-astro-081915-023307 2016

  42. [42]

    Kristiansen, M. H. K., Rappaport, S. A., Vanderburg, A. M., et al. 2022, PASP, 134, 074401, doi: 10.1088/1538-3873/ac6e06

    work page doi:10.1088/1538-3873/ac6e06 2022

  43. [43]

    Research Notes of the American Astronomical Society , keywords =

    Kunimoto, M., Tey, E., Fong, W., et al. 2022, Research Notes of the American Astronomical Society, 6, 236, doi: 10.3847/2515-5172/aca158

    work page doi:10.3847/2515-5172/aca158 2022

  44. [44]

    Research Notes of the American Astronomical Society , keywords =

    Kunimoto, M., Huang, C., Tey, E., et al. 2021, Research Notes of the American Astronomical Society, 5, 234, doi: 10.3847/2515-5172/ac2ef0 Lightkurve Collaboration, Cardoso, J. V. d. M., Hedges, C., et al. 2018, Lightkurve: Kepler and TESS time series analysis in Python,, Astrophysics Source Code Library http://ascl.net/1812.013

    work page doi:10.3847/2515-5172/ac2ef0 2021

  45. [45]

    2010, in Proceedings of the 9th Python in Science Conference, ed

    McKinney, W. 2010, in Proceedings of the 9th Python in Science Conference, ed. S. van der Walt & J. Millman, 51 – 56

    work page 2010

  46. [46]

    R., et al

    Mitnyan, T., Borkovits, T., Czavalinga, D. R., et al. 2024, A&A, 685, A43, doi: 10.1051/0004-6361/202348909

    work page doi:10.1051/0004-6361/202348909 2024

  47. [47]

    Maxted, P. F. L. 2020, MNRAS, 498, 6034, doi: 10.1093/mnras/staa2762

    work page doi:10.1093/mnras/staa2762 2020

  48. [48]

    Astronomy and Astrophysics Supplement Series , author =

    Ochsenbein, F., Bauer, P., & Marcout, J. 2000, A&AS, 143, 23, doi: 10.1051/aas:2000169

    work page doi:10.1051/aas:2000169 2000

  49. [49]

    2011 , keywords =

    Paxton, B., Bildsten, L., Dotter, A., et al. 2011, ApJS, 192, 3, doi: 10.1088/0067-0049/192/1/3

    work page doi:10.1088/0067-0049/192/1/3 2011

  50. [50]

    2013 , keywords =

    Paxton, B., Cantiello, M., Arras, P., et al. 2013, ApJS, 208, 4, doi: 10.1088/0067-0049/208/1/4

    work page internal anchor Pith review doi:10.1088/0067-0049/208/1/4 2013

  51. [51]

    2015 , keywords =

    Paxton, B., Marchant, P., Schwab, J., et al. 2015, ApJS, 220, 15, doi: 10.1088/0067-0049/220/1/15 P´ erez, F., & Granger, B. E. 2007, Computing in Science and Engineering, 9, 21, doi: 10.1109/MCSE.2007.53

    work page internal anchor Pith review doi:10.1088/0067-0049/220/1/15 2015

  52. [52]

    P., Kostov, V

    Powell, B. P., Kostov, V. B., & Tokovinin, A. 2023, MNRAS, 524, 4296, doi: 10.1093/mnras/stad2065

    work page doi:10.1093/mnras/stad2065 2023

  53. [53]

    P., Kostov, V

    Powell, B. P., Kostov, V. B., Rappaport, S. A., et al. 2021, AJ, 161, 162, doi: 10.3847/1538-3881/abddb5 22

    work page doi:10.3847/1538-3881/abddb5 2021

  54. [54]

    2013, ApJ, 768, 33, doi: 10.1088/0004-637X/768/1/33

    Rappaport, S., Deck, K., Levine, A., et al. 2013, ApJ, 768, 33, doi: 10.1088/0004-637X/768/1/33

    work page doi:10.1088/0004-637x/768/1/33 2013

  55. [55]

    A., Borkovits, T., Gagliano, R., et al

    Rappaport, S. A., Borkovits, T., Gagliano, R., et al. 2022, MNRAS, 513, 4341, doi: 10.1093/mnras/stac957

    work page doi:10.1093/mnras/stac957 2022

  56. [56]

    A., Borkovits, T., Gagliano, R., et al

    Rappaport, S. A., Borkovits, T., Gagliano, R., et al. 2023, MNRAS, 521, 558, doi: 10.1093/mnras/stad367

    work page doi:10.1093/mnras/stad367 2023

  57. [58]

    A., Borkovits, T., Mitnyan, T., et al

    Rappaport, S. A., Borkovits, T., Mitnyan, T., et al. 2024b, A&A, 686, A27, doi: 10.1051/0004-6361/202449273

    work page doi:10.1051/0004-6361/202449273

  58. [59]

    2012, Astronomy & Astrophysics, 537, A128

    Rein, H., & Liu, S.-F. 2012, Astronomy & Astrophysics, 537, A128

    work page 2012

  59. [60]

    Rein, H., & Spiegel, D. S. 2015, MNRAS, 446, 1424, doi: 10.1093/mnras/stu2164

    work page doi:10.1093/mnras/stu2164 2015

  60. [61]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003, doi: 10.1117/1.JATIS.1.1.014003

    work page internal anchor Pith review doi:10.1117/1.jatis.1.1.014003 2015

  61. [62]

    2021, arXiv e-prints, arXiv:2103.10285

    Schmitt, A., & Vanderburg, A. 2021, arXiv e-prints, arXiv:2103.10285. https://arxiv.org/abs/2103.10285

    work page arXiv 2021

  62. [63]

    R., Hartman, J

    Schmitt, A. R., Hartman, J. D., & Kipping, D. M. 2019, arXiv e-prints, arXiv:1910.08034. https://arxiv.org/abs/1910.08034

    work page arXiv 2019

  63. [64]

    G., Oelkers, R

    Stassun, K. G., Oelkers, R. J., Paegert, M., et al. 2019, AJ, 158, 138, doi: 10.3847/1538-3881/ab3467

    work page doi:10.3847/1538-3881/ab3467 2019

  64. [65]

    1997, Journal of Global Optimization, 11, 341, doi: 10.1023/A:1008202821328

    Storn, R., & Price, K. 1997, Journal of Global Optimization, 11, 341, doi: 10.1023/A:1008202821328

    work page doi:10.1023/a:1008202821328 1997

  65. [66]

    H., & Fur´ esz, G

    Szentgyorgyi, A. H., & Fur´ esz, G. 2007, in Revista Mexicana de Astronomia y Astrofisica Conference Series, Vol. 28, Revista Mexicana de Astronomia y Astrofisica Conference Series, ed. S. Kurtz, 129–133

    work page 2007

  66. [67]

    J., Kratter, K

    Tobin, J. J., Kratter, K. M., Persson, M. V., et al. 2016, Nature, 538, 483, doi: 10.1038/nature20094

    work page doi:10.1038/nature20094 2016

  67. [68]

    2017, ApJ, 844, 103, doi: 10.3847/1538-4357/aa7746

    Tokovinin, A. 2017, ApJ, 844, 103, doi: 10.3847/1538-4357/aa7746

    work page doi:10.3847/1538-4357/aa7746 2017

  68. [69]

    2022, ApJ, 926, 1, doi: 10.3847/1538-4357/ac4584

    Tokovinin, A. 2022, ApJ, 926, 1, doi: 10.3847/1538-4357/ac4584

    work page doi:10.3847/1538-4357/ac4584 2022

  69. [70]

    2023, AJ, 165, 165, doi: 10.3847/1538-3881/acbf32

    Tokovinin, A. 2023, AJ, 165, 165, doi: 10.3847/1538-3881/acbf32

    work page doi:10.3847/1538-3881/acbf32 2023

  70. [71]

    2025, AJ, 169, 124, doi: 10.3847/1538-3881/ada3c6

    Tokovinin, A. 2025, AJ, 169, 124, doi: 10.3847/1538-3881/ada3c6

    work page doi:10.3847/1538-3881/ada3c6 2025

  71. [72]

    Tokovinin, A., & Latham, D. W. 2020, AJ, 160, 251, doi: 10.3847/1538-3881/abbad4

    work page doi:10.3847/1538-3881/abbad4 2020

  72. [73]

    2016, Computational Astrophysics and Cosmology, 3, 6, doi: 10.1186/s40668-016-0019-0

    Toonen, S., Hamers, A., & Portegies Zwart, S. 2016, Computational Astrophysics and Cosmology, 3, 6, doi: 10.1186/s40668-016-0019-0

    work page doi:10.1186/s40668-016-0019-0 2016

  73. [74]

    Torres, G., Neuh¨ auser, R., & Guenther, E. W. 2002, AJ, 123, 1701, doi: 10.1086/339178

    work page doi:10.1086/339178 2002

  74. [75]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and van der Walt, Stéfan J

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, doi: https://doi.org/10.1038/s41592-019-0686-2

    work page doi:10.1038/s41592-019-0686-2 2020

  75. [76]

    The Astrophysical Journal , author =

    Zucker, S., & Mazeh, T. 1994, ApJ, 420, 806, doi: 10.1086/173605

    work page doi:10.1086/173605 1994

  76. [77]

    1995, ApJ, 452, 863, doi: 10.1086/176354

    Zucker, S., Torres, G., & Mazeh, T. 1995, ApJ, 452, 863, doi: 10.1086/176354

    work page doi:10.1086/176354 1995