TESS Giants Transiting Giants. II. The Hottest Jupiters Orbiting Evolved Stars

Grunblatt, Samuel K. and Saunders, Nicholas and Sun, Meng and Chontos, Ashley and Soares-Furtado, Melinda and Eisner, Nora and Pereira, Filipe and Komacek, Thaddeus and Huber, Daniel and Collins, Karen and Wang, Gavin and Stockdale, Chris and Quinn, Samuel N. and Tronsgaard, Rene and Zhou, George ORCID: https://orcid.org/0000-0002-4891-3517 and Nowak, Grzegorz and Deeg, Hans J. and Ciardi, David R. and Boyle, Andrew and Rice, Malena and Dai, Fei and Blunt, Sarah and Van Zandt, Judah and Beard, Corey and Akana Murphy, Joseph M. and Dalba, Paul A. and Lubin, Jack and Polanski, Alex and Brinkman, Casey Lynn and Howard, Andrew W. and Buchhave, Lars A. and Angus, Ruth and Ricker, George R. and Jenkins, Jon M. and Wohler, Bill and Goeke, Robert F. and Levine, Alan M. and Colon, Knicole D. and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Kunimoto, Michelle and Shporer, Avi and Latham, David W. and Seager, Sara and Vanderspek, Roland K. and Winn, Joshua N. (2022) TESS Giants Transiting Giants. II. The Hottest Jupiters Orbiting Evolved Stars. The Astronomical Journal, 163 (3):120. pp. 1-16. ISSN 0004-6256

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Abstract

Giant planets on short-period orbits are predicted to be inflated and eventually engulfed by their host stars. However, the detailed timescales and stages of these processes are not well known. Here, we present the discovery of three hot Jupiters (P < 10 days) orbiting evolved, intermediate-mass stars (M ⋆ ≈ 1.5 M ⊙, 2 R ⊙ < R ⋆ < 5 R ⊙). By combining TESS photometry with ground-based photometry and radial velocity measurements, we report masses and radii for these three planets of between 0.4 and 1.8 M J and 0.8 and 1.8 R J. TOI-2337b has the shortest period (P = 2.99432 ± 0.00008 days) of any planet discovered around a red giant star to date. Both TOI-4329b and TOI-2669b appear to be inflated, but TOI-2337b does not show any sign of inflation. The large radii and relatively low masses of TOI-4329b and TOI-2669b place them among the lowest density hot Jupiters currently known, while TOI-2337b is conversely one of the highest. All three planets have orbital eccentricities of below 0.2. The large spread in radii for these systems implies that planet inflation has a complex dependence on planet mass, radius, incident flux, and orbital properties. We predict that TOI-2337b has the shortest orbital decay timescale of any planet currently known, but do not detect any orbital decay in this system. Transmission spectroscopy of TOI-4329b would provide a favorable opportunity for the detection of water, carbon dioxide, and carbon monoxide features in the atmosphere of a planet orbiting an evolved star, and could yield new information about planet formation and atmospheric evolution.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Date Deposited: 12 May 2022 05:29
Last Modified: 12 May 2022 05:29
Uncontrolled Keywords: Exoplanet astronomy (486); Star-planet interactions (2177); Stellar evolution (1599); Astrophysics - Earth and Planetary Astrophysics
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Socio-Economic Objectives (2020): 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences
Funding Details:
Identification Number or DOI: https://doi.org/10.3847/1538-3881/ac4972
URI: http://eprints.usq.edu.au/id/eprint/48448

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