A Highly Eccentric Warm Jupiter Orbiting TIC 237913194
Martin Schlecker, D. Kossakowski, Rafael Brahm, Néstor Espinoza, Thomas Henning, L. Carone, Karan Molaverdikhani, Trifon Trifonov, P. Mollière, Mélissa J. Hobson, Andrés Jordán, Felipe Rojas, Hubert Klahr, P. Sarkis, G. Á. Bakos, W. Bhatti, D. J. Osip, V. Suc, G. Ricker, R. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, J. Villaseñor, Mark E. Rose, David R. Rodriguez, Joseph E. Rodriguez, Samuel N. Quinn, Avi Shporer
Abstract
Abstract The orbital parameters of warm Jupiters serve as a record of their formation history, providing constraints on formation scenarios for giant planets on close and intermediate orbits. Here, we report the discovery of TIC 237913194b, detected in full-frame images from Sectors 1 and 2 of the Transiting Exoplanet Survey Satellite (TESS), ground-based photometry (Chilean–Hungarian Automated Telescope, Las Cumbres Observatory Global Telescope), and Fiber-fed Extended Range Optical Spectrograph radial velocity time series. We constrain its mass to = and its radius to = , implying a bulk density similar to Neptune’s. It orbits a G-type star ( = , V = 12.1 mag) with a period of 15.17 days on one of the most eccentric orbits of all known warm giants ( e ≈ 0.58). This extreme dynamical state points to a past interaction with an additional, undetected massive companion. A tidal evolution analysis showed a large tidal dissipation timescale, suggesting that the planet is not a progenitor for a hot Jupiter caught during its high-eccentricity migration. TIC 237913194b further represents an attractive opportunity to study the energy deposition and redistribution in the atmosphere of a warm Jupiter with high eccentricity.