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A Highly Eccentric Warm Jupiter Orbiting TIC 237913194

  • Authors: Martin Schlecker, Diana Kossakowski, Rafael Brahm, Néstor Espinoza, Thomas Henning, Ludmila Carone, Karan Molaverdikhani, Trifon Trifonov, Paul Mollière, Melissa J. Hobson, Andrés Jordán, Felipe I. Rojas, Hubert Klahr, Paula Sarkis, Gáspár Á. Bakos, Waqas Bhatti, David Osip, Vincent Suc, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Jesus Noel Villaseñor, Mark E. Rose, David R. Rodriguez, Joseph E. Rodriguez, Samuel N. Quinn, and Avi Shporer

2020 The Astronomical Journal 160 275.

  • Provider: AAS Journals

Caption: Figure 7.

Comparison to other well-characterized warm Jupiters. Left: period–eccentricity plot of transiting exoplanets with periods of 1–100 days and measured eccentricity from the TEPCat catalog (Southworth 2011). Marker sizes scale with planet mass. With e=0.58, TIC 237913194b occupies the 98th percentile in this population and contributes to a sparse sample of planets with very high eccentricities.   Right: mass–radius diagram of warm (﹩P=10\mbox{--}100\,\mathrm{days}﹩) planets from the same catalog. The color of the markers represent the equilibrium temperatures of the planets, and dashed gray lines are isodensity curves of 0.3, 3, and 30 g cm−3, respectively. The solid blue line marks the predicted mass–radius relation for giant planets with a 10 ﹩{M}_{\oplus }﹩ core (Fortney et al. 2007). TIC 237913194b lies very close to this line. The error bars for its mass are too small to be seen.

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