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The K2-ESPRINT Project V: a short-period giant planet orbiting a subgiant star | | Vincent Van Eylen
; Simon Albrecht
; Davide Gandolfi
; Fei Dai
; Joshua N. Winn
; Teriyuki Hirano
; Norio Narita
; Hans Bruntt
; Jorge Prieto-Arranz
; Victor J. S. Bejar
; Grzegorz Nowak
; Mikkel N. Lund
; Enric Palle
; Ignasi Ribas
; Roberto Sanchis-Ojeda
; Liang Yu
; Pamela Arriagada
; R. Paul Butler
; Jeffrey D. Crane
; Rasmus Handberg
; Hans Deeg
; Jens Jessen-Hansen
; John A. Johnson
; David Nespral
; Leslie Rogers
; Tsuguru Ryu
; Stephen Shectman
; Tushar Shrotriya
; Ditte Slumstrup
; Yoichi Takeda
; Johanna Teske
; Ian Thompson
; Andrew Vanderburg
; Robert Wittenmyer
; | | Date: |
30 May 2016 | | Abstract: | We report on the discovery and characterization of the transiting planet
K2-39b (EPIC 206247743b). With an orbital period of 4.6 days, it is the
shortest-period planet orbiting a subgiant star known to date. Such planets are
rare, with only a handful of known cases. The reason for this is poorly
understood, but may reflect differences in planet occurrence around the
relatively high-mass stars that have been surveyed, or may be the result of
tidal destruction of such planets. K2-39 is an evolved star with a
spectroscopically derived stellar radius and mass of
$3.88^{+0.48}_{-0.42}~mathrm{R_odot}$ and
$1.53^{+0.13}_{-0.12}~mathrm{M_odot}$, respectively, and a very close-in
transiting planet, with $a/R_star = 3.4$. Radial velocity (RV) follow-up using
the HARPS, FIES and PFS instruments leads to a planetary mass of
$50.3^{+9.7}_{-9.4}~mathrm{M_oplus}$. In combination with a radius
measurement of $8.3 pm 1.1~mathrm{R_oplus}$, this results in a mean
planetary density of $0.50^{+0.29}_{-0.17}$ g~cm$^{-3}$. We furthermore
discover a long-term RV trend, which may be caused by a long-period planet or
stellar companion. Because K2-39b has a short orbital period, its existence
makes it seem unlikely that tidal destruction is wholly responsible for the
differences in planet populations around subgiant and main-sequence stars.
Future monitoring of the transits of this system may enable the detection of
period decay and constrain the tidal dissipation rates of subgiant stars. | | Source: | arXiv, 1605.9180 | | Services: | Forum | Review | PDF | Favorites | |
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