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TESS Giants Transiting Giants. III. An Eccentric Warm Jupiter Supports a Period-Eccentricity Relation for Giant Planets Transiting Evolved Starsстатья
Статья опубликована в высокорейтинговом журнале
Статья опубликована в журнале из списка Web of Science и/или Scopus- Авторы: Grunblatt Samuel K., Saunders Nicholas, Chontos Ashley, Hattori Soichiro, Veras Dimitri, Huber Daniel, Angus Ruth, Rice Malena, Breivik Katelyn, Blunt Sarah, Giacalone Steven, Lubin Jack, Isaacson Howard, Howard Andrew W., Ciardi David R., Safonov Boris S., Strakhov Ivan A., Latham David W., Bieryla Allyson, Ricker George R., Jenkins Jon M., Tenenbaum Peter, Shporer Avi, Morgan Edward H., Kostov Veselin, Osborn Hugh P., Dragomir Diana, Seager Sara, Vanderspek Roland K., Winn Joshua N.
- Журнал: Astronomical Journal
- Том: 165
- Номер: 2
- Год издания: 2023
- Издательство: American Astronomical Society
- Местоположение издательства: United States
- Первая страница: 44
- DOI: 10.3847/1538-3881/aca670
- Аннотация: 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+blog10(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.
- Добавил в систему: Сафонов Борис Сергеевич