Discovery and characterization of two Neptune-mass planets orbiting HD 212729 with TESS

Armstrong, David J.; Osborn, Ares; Adibekyan, Vardan; Delgado-Mena, Elisa; Hojjatpanah, Saeed; Howell, Steve B.; Hoyer, Sergio; Knierim, Henrik; Sousa, Sérgio G.; Stassun, Keivan G.; Veras, Dimitri; Anderson, David R.; Bayliss, Daniel; Bouchy, François; Burke, Christopher J.; Christiansen, Jessie L.; Dumusque, Xavier; Keniger, Marcelo Aron Fetzner; Hadjigeorghiou, Andreas; Hawthorn, Faith; Helled, Ravit; Jenkins, Jon M.; Latham, David W.; Lillo-Box, Jorge; Nielsen, Louise D.; Osborn, Hugh P.; Rodrigues, José; Rodriguez, David; Santos, Nuno C.; Seager, Sara; Strøm, Paul A.; Torres, Guillermo; Twicken, Joseph D.; Udry, Stephane; Wheatley, Peter J.; Winn, Joshua N.

doi:10.1093/mnras/stad2183

Title: Discovery and characterization of two Neptune-mass planets orbiting HD 212729 with TESS

Journal Article · 19 July 2023 · Monthly Notices of the Royal Astronomical Society

DOI: https://doi.org/10.1093/mnras/stad2183 · OSTI ID:1994424

;

; Adibekyan, Vardan; Delgado-Mena, Elisa; Hojjatpanah, Saeed; Howell, Steve B.;

; Knierim, Henrik;

;

; Anderson, David R.; Bayliss, Daniel; Bouchy, François; Burke, Christopher J.; Christiansen, Jessie L.; Dumusque, Xavier; Keniger, Marcelo Aron Fetzner; Hadjigeorghiou, Andreas; Hawthorn, Faith more »

ABSTRACT We report the discovery of two exoplanets orbiting around HD 212729 (TOI 1052, TIC 317060587), a Teff = 6146 K star with V = 9.51 observed by TESS in Sectors 1 and 13. One exoplanet, TOI-1052b, is Neptune-mass and transits the star, and an additional planet TOI-1052c is observed in radial velocities but not seen to transit. We confirm the planetary nature of TOI-1052b using precise radial velocity observations from HARPS and determined its parameters in a joint RV and photometry analysis. TOI-1052b has a radius of $$2.87^{+0.29}_{-0.24}$$ R⊕, a mass of 16.9 ± 1.7 M⊕, and an orbital period of 9.14 d. TOI-1052c does not show any transits in the TESS data, and has a minimum mass of $$34.3^{+4.1}_{-3.7}$$ M⊕ and an orbital period of 35.8 d, placing it just interior to the 4:1 mean-motion resonance. Both planets are best fit by relatively high but only marginally significant eccentricities of $$0.18^{+0.09}_{-0.07}$$ for planet b and $$0.24^{+0.09}_{-0.08}$$ for planet c. We perform a dynamical analysis and internal structure model of the planets as well as deriving stellar parameters and chemical abundances. The mean density of TOI-1052b is $$3.9^{+1.7}_{-1.3}$$ g cm−3 consistent with an internal structure similar to Neptune. A nearby star is observed in Gaia DR3 with the same distance and proper motion as TOI-1052, at a sky projected separation of $$\scriptstyle \sim$$1500 au, making this a potential wide binary star system.

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Sponsoring Organization:: USDOE Office of Nuclear Energy (NE), Nuclear Fuel Cycle and Supply Chain

OSTI ID:: 1994424

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 4 Vol. 524; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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