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TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet

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    0575157 - ASÚ 2024 RIV FR eng J - Článek v odborném periodiku
    Korth, J. - Gandolfi, D. - Šubjak, Ján - Kabáth, Petr … celkem 62 autorů
    TOI-1130: A photodynamical analysis of a hot Jupiter in resonance with an inner low-mass planet.
    Astronomy & Astrophysics. Roč. 675, July (2023), č. článku A115. ISSN 0004-6361. E-ISSN 1432-0746
    Grant CEP: GA MŠMT(CZ) LTT20015
    Institucionální podpora: RVO:67985815
    Klíčová slova: planetary systems * planets and satellites * photometric techniques
    Obor OECD: Astronomy (including astrophysics,space science)
    Impakt faktor: 6.5, rok: 2022
    Způsob publikování: Open access

    The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c on an 8.4-day orbit that is accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We performed a photodynamical modeling of the HARPS and PFS RVs, along with transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program (TFOP). We determined the planet masses and radii of TOI-1130 b and TOI1130 c to be Mb = 19.28 +/- 0.97 M. and Rb = 3.56 +/- 0.13 R., and Mc = 325.59 +/- 5.59 M. and Rc = 13.32+1.551.41 R., respectively. We have spectroscopically confirmed the existence of TOI-1130 b, which had previously only been validated. We find that the two planets have orbits with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small, yet growing population of hot Jupiters with an inner low-mass planet that poses a challenge to the pathway scenario for hot Jupiter formation. We also detected a linear RV trend that is possibly due to the presence of an outer massive companion.
    Trvalý link: https://hdl.handle.net/11104/0345819

     
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