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TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars

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Title: TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period−Eccentricity Relation for Giant Planets Transiting Evolved Stars
Authors: Samuel K. Grunblatt, Nicholas Saunders, Ashley Chontos, Soichiro Hattori, Dimitri Veras, Daniel Huber, Ruth Angus, Malena Rice, Katelyn Breivik, Sarah Blunt, Steven Giacalone, Jack Lubin, Howard Isaacson, Andrew W. Howard, David R. Ciardi, Boris S. Safonov, Ivan A. Strakhov, David W. Latham, Allyson Bieryla, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, Avi Shporer, Edward H. Morgan, Veselin Kostov, Hugh P. Osborn, Diana Dragomir, Sara Seager, Roland K. Vanderspek, Joshua N. Winn
Source: The Astronomical Journal, Vol 165, Iss 2, p 44 (2023)
Publisher Information: IOP Publishing, 2023.
Publication Year: 2023
Collection: LCC:Astronomy
Subject Terms: Exoplanets, Stellar evolution, Star-planet interactions, Transits, Extrasolar gaseous giant planets, Astronomy, QB1-991
More Details: The fate of planets around rapidly evolving stars is not well understood. Previous studies have suggested that, relative to the main-sequence population, planets transiting evolved stars ( P < 100 days) tend to have more eccentric orbits. Here we present the discovery of TOI-4582 b, a ${0.94}_{-0.12}^{+0.09}$ R _J , 0.53 ± 0.05 M _J planet orbiting an intermediate-mass subgiant star every 31.034 days. We find that this planet is also on a significantly eccentric orbit ( e = 0.51 ± 0.05). We then compare the population of planets found transiting evolved (log g < 3.8) stars to the population of planets transiting main-sequence stars. We find that the rate at which median orbital eccentricity grows with period is significantly higher for evolved star systems than for otherwise similar main-sequence systems. In general, we observe that mean planet eccentricity 〈 e 〉 = a + b log _10 ( P ) for the evolved population with significant orbital eccentricity where a = −0.18 ± 0.08 and b = 0.38 ± 0.06, significantly distinct from the main-sequence planetary system population. This trend is seen even after controlling for stellar mass and metallicity. These systems do not appear to represent a steady evolution pathway from eccentric, long-period planetary orbits to circular, short-period orbits, as orbital model comparisons suggest that inspiral timescales are uncorrelated with orbital separation or eccentricity. Characterization of additional evolved planetary systems will distinguish effects of stellar evolution from those of stellar mass and composition.
Document Type: article
File Description: electronic resource
Language: English
ISSN: 1538-3881
Relation: https://doaj.org/toc/1538-3881
DOI: 10.3847/1538-3881/aca670
Access URL: https://doaj.org/article/c012714a9bd94bb69cd81702d7d48771
Accession Number: edsdoj.012714a9bd94bb69cd81702d7d48771
Database: Directory of Open Access Journals
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  Data: The fate of planets around rapidly evolving stars is not well understood. Previous studies have suggested that, relative to the main-sequence population, planets transiting evolved stars ( P &lt; 100 days) tend to have more eccentric orbits. Here we present the discovery of TOI-4582 b, a ${0.94}_{-0.12}^{+0.09}$ R _J , 0.53 &#177; 0.05 M _J planet orbiting an intermediate-mass subgiant star every 31.034 days. We find that this planet is also on a significantly eccentric orbit ( e = 0.51 &#177; 0.05). We then compare the population of planets found transiting evolved (log g &lt; 3.8) stars to the population of planets transiting main-sequence stars. We find that the rate at which median orbital eccentricity grows with period is significantly higher for evolved star systems than for otherwise similar main-sequence systems. In general, we observe that mean planet eccentricity 〈 e 〉 = a + b log _10 ( P ) for the evolved population with significant orbital eccentricity where a = −0.18 &#177; 0.08 and b = 0.38 &#177; 0.06, significantly distinct from the main-sequence planetary system population. This trend is seen even after controlling for stellar mass and metallicity. These systems do not appear to represent a steady evolution pathway from eccentric, long-period planetary orbits to circular, short-period orbits, as orbital model comparisons suggest that inspiral timescales are uncorrelated with orbital separation or eccentricity. Characterization of additional evolved planetary systems will distinguish effects of stellar evolution from those of stellar mass and composition.
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