TESS giants transiting giants V – two hot Jupiters orbiting red giant hosts

Author:

Pereira Filipe12ORCID,Grunblatt Samuel K345,Psaridi Angelica6,Campante Tiago L12ORCID,Cunha Margarida S12ORCID,Santos Nuno C12,Bossini Diego1,Thorngren Daniel5,Hellier Coel7,Bouchy François6,Lendl Monika6ORCID,Mounzer Dany6,Udry Stéphane6,Beard Corey8,Brinkman Casey L9ORCID,Isaacson Howard1011,Quinn Samuel N12,Tyler Dakotah13,Zhou George11,Howell Steve B14,Howard Andrew W15,Jenkins Jon M14,Seager Sara161718,Vanderspek Roland K16,Winn Joshua N19,Saunders Nicholas9,Huber Daniel920

Affiliation:

1. Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP , Rua das Estrelas, P-4150-762 Porto , Portugal

2. Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto , Rua do Campo Alegre, P-4169-007 Porto , Portugal

3. American Museum of Natural History , 200 Central Park West, Manhattan, NY 10024 , USA

4. Center for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, Manhattan, NY 10010 , USA

5. Department of Physics and Astronomy, Johns Hopkins University , Baltimore, MD , USA

6. Observatoire Astronomique de l’Université de Genève , Chemin Pegasi 51, CH-1290 Versoix , Switzerland

7. Astrophysics Group, Keele University , Staffordshire ST5 5BG , UK

8. Department of Physics and Astronomy, University of California , Irvine, Irvine, CA 92697 , USA

9. Institute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822 USA

10. Institute for Astronomy, University of California Berkeley , Berkeley, CA 94720 , USA

11. Centre for Astrophysics , University of Southern Queensland, West Street, Toowoomba, QLD 4350 , Australia

12. Center for Astrophysics | Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138 , USA

13. Department of Physics and Astronomy, University of California Los Angeles , Los Angeles, CA 90095 , USA

14. NASA Ames Research Center , Moffett Field, CA 94035 , USA

15. Department of Astronomy, California Institute of Technology , Pasadena, CA 91125 , USA

16. Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139 , USA

17. Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology , Cambridge, MA 02139 , USA

18. Department of Aeronautics and Astronautics, MIT , 77 Massachusetts Avenue, Cambridge, MA 02139 , USA

19. Department of Astrophysical Sciences, Princeton University , Princeton, NJ 08544 , USA

20. Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney , NSW 2006 , Australia

Abstract

ABSTRACT In this work, we present the discovery and confirmation of two hot Jupiters orbiting red giant stars, TOI-4377 b and TOI-4551 b, observed by Transiting Exoplanet Survey Satellite in the Southern ecliptic hemisphere and later followed-up with radial-velocity (RV) observations. For TOI-4377 b, we report a mass of $0.957^{+0.089}_{-0.087} \ M_\mathrm{J}$ and a inflated radius of 1.348 ± 0.081 RJ orbiting an evolved intermediate-mass star (1.36 M⊙ and 3.52 R⊙; TIC 394918211) on a period of of 4.378 d. For TOI-4551 b, we report a mass of 1.49 ± 0.13 MJ and a radius that is not obviously inflated of $1.058^{+0.110}_{-0.062} \ R_\mathrm{J}$, also orbiting an evolved intermediate-mass star (1.31 M⊙ and 3.55 R⊙; TIC 204650483) on a period of 9.956 d. We place both planets in context of known systems with hot Jupiters orbiting evolved hosts, and note that both planets follow the observed trend of the known stellar incident flux-planetary radius relation observed for these short-period giants. Additionally, we produce planetary interior models to estimate the heating efficiency with which stellar incident flux is deposited in the planet’s interior, estimating values of $1.91 \pm 0.48~{{\ \rm per\ cent}}$ and $2.19 \pm 0.45~{{\ \rm per\ cent}}$ for TOI-4377 b and TOI-4551 b, respectively. These values are in line with the known population of hot Jupiters, including hot Jupiters orbiting main-sequence hosts, which suggests that the radii of our planets have re-inflated in step with their parent star’s brightening as they evolved into the post-main sequence. Finally, we evaluate the potential to observe orbital decay in both systems.

Funder

FCT

FEDER

National Aeronautics and Space Administration

ERC

Swiss National Science Foundation

MIT

University of Geneva

National Science Foundation

Alfred P. Sloan Foundation

Australian Research Council

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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