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Planet Hunters TESS V: a planetary system around a binary star, including a mini-Neptune in the habitable zone

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arxiv 2404.18997 v1 pith:S5OONEU4 submitted 2024-04-29 astro-ph.EP

Nora L. Eisner , Samuel K. Grunblatt , Oscar Barragán , Thea H. Faridani , Chris Lintott , Suzanne Aigrain , Cole Johnston , Ian R.Mason
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Keivan G. Stassun Megan Bedell Andrew W. Boyle David R. Ciardi Catherine A. Clark Guillaume Hebrard David W. Hogg Steve B. Howell Baptiste Klein Joe Llama Joshua N. Winn Lily L. Zhao Joseph M. Akana Murphy Corey Beard Casey L. Brinkman Ashley Chontos Pia Cortes-Zuleta Xavier Delfosse Steven Giacalone Emily A. Gilbert Neda Heidari Rae Holcomb Jon M. Jenkins Flavien Kiefer Jack Lubin Eder Martioli Alex S. Polanski Nicholas Saunders Sara Seager Avi Shporer Dakotah Tyler Judah Van Zandt Safaa Alhassan Daval J. Amratlal Lais I. Antonel Simon L. S. Bentzen Milton K. D. Bosch David Bundy Itayi Chitsiga Jérôme F. Delaunay Xavier Doisy Richard Ferstenou Mark Fyn{o} James M. Geary Gerry Haynaly Pete Hermes Marc Huten Sam Lee Paul Metcalfe Garry J. Pennell Joanna Puszkarska Thomas Schäfer Lisa Stiller Christopher Tanner Allan Tarr Andrew Wilkinson
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We report on the discovery and validation of a transiting long-period mini-Neptune orbiting a bright (V = 9.0 mag) G dwarf (TOI 4633; R = 1.05 RSun, M = 1.10 MSun). The planet was identified in data from the Transiting Exoplanet Survey Satellite by citizen scientists taking part in the Planet Hunters TESS project. Modeling of the transit events yields an orbital period of 271.9445 +/- 0.0040 days and radius of 3.2 +/- 0.20 REarth. The Earth-like orbital period and an incident flux of 1.56 +/- 0.2 places it in the optimistic habitable zone around the star. Doppler spectroscopy of the system allowed us to place an upper mass limit on the transiting planet and revealed a non-transiting planet candidate in the system with a period of 34.15 +/- 0.15 days. Furthermore, the combination of archival data dating back to 1905 with new high angular resolution imaging revealed a stellar companion orbiting the primary star with an orbital period of around 230 years and an eccentricity of about 0.9. The long period of the transiting planet, combined with the high eccentricity and close approach of the companion star makes this a valuable system for testing the formation and stability of planets in binary systems.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Planet formation and long-term stability in a very eccentric stellar binary

    astro-ph.EP 2025-01 accept novelty 6.0 of 10

    Long-term N-body simulations indicate that the mini-Neptune TOI 4633c is only stable over the system's 1.3 Gyr age if its orbit is retrograde relative to the highly eccentric stellar binary.

  2. From stellar light to astrophysical insight: automating variable star research with machine learning

    astro-ph.IM 2025-07 unverdicted

    An invited review of machine learning for automated variable star research, covering data cleaning, variability classification, stellar parameter inference, and foundation models.

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