Kavli Affiliate: George Ricker
| First 5 Authors: Ilaria Carleo, Oscar Barrágan, Carina M. Persson, Malcolm Fridlund, Kristine W. F. Lam
| Summary:
Hot and warm Jupiters might have undergone the same formation and evolution
path, but the two populations exhibit different distributions of orbital
parameters, challenging our understanding on their actual origin. The present
work, which is the results of our warm Jupiters survey carried out with the
CHIRON spectrograph within the KESPRINT collaboration, aims to address this
challenge by studying two planets that could help bridge the gap between the
two populations. We report the confirmation and mass determination of a hot
Jupiter (orbital period shorter than 10 days), TOI-2420,b, and a warm Jupiter,
TOI-2485,b. We performed a joint analysis using a wide variety of spectral and
photometric data in order to characterize these planetary systems. We found
that TOI-2420,b has an orbital period of P$_{rm b}$=5.8 days, a mass of
M$_{rm b}$=0.9 M$_{rm J}$ and a radius of R$_{rm b}$=1.3 R$_{rm J}$, with a
planetary density of 0.477 gc; while TOI-2485,b has an orbital period of
P$_{rm b}$=11.2 days, a mass of M$_{rm b}$=2.4 M$_{rm J}$ and a radius of
R$_{rm b}$=1.1 R$_{rm J}$ with density 2.36 gc. With current parameters, the
migration history for TOI-2420,b and TOI-2485,b is unclear: the
high-eccentricity migration scenarios cannot be ruled out, and TOI-2485,b’s
characteristics may rather support this scenario.
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