Super-Earth of 8 M ⊕ in a 2.2-day orbit around the K5V star K2-216

Persson, C. M.; Fridlund, M.; Barragan, O.; Dai, F.; Gandolfi, D.; Hatzes, A. P.; Hirano, T.; Grziwa, S.; Korth, J.; Prieto-Arranz, J.; Fossati, L.; Van Eylen, V.; Justesen, A. B.; Livingston, J.; Kubyshkina, D.; Deeg, H. J.; Guenther, E. W.; Nowak, G.; Cabrera, J.; Eigmoller, Ph.; Csizmadia, Sz.; Smith, A. M. S.; Erikson, A.; Albrecht, S.; Sobrino, ANNA MARIA; Cochran, W. D.; Endl, M.; Esposito, M.; Fukui, A.; Heeren, P.; Hidalgo, D.; Hjorth, M.; Kuzuhara, M.; Narita, N.; Nespral, D.; Palle, E.; Patzold, M.; Rauer, H.; Rodler, F.; Winn, J. N.

doi:10.1051/0004-6361/201832867

Context. Although thousands of exoplanets have been discovered to date, far fewer have been fully characterised, in particular super-Earths. The KESPRINT consortium identified K2-216 as a planetary candidate host star in the K2 space mission Campaign 8 field with a transiting super-Earth. The planet has recently been validated as well. Aims. Our aim was to confirm the detection and derive the main physical characteristics of K2-216 b, including the mass. Methods. We performed a series of follow-up observations: high-resolution imaging with the FastCam camera at the TCS and the Infrared Camera and Spectrograph at Subaru, and high-resolution spectroscopy with HARPS (La Silla), HARPS-N (TNG), and FIES (NOT). The stellar spectra were analyzed with the SpecMatch-Emp and SME codes to derive the fundamental stellar properties. We analyzed the K2 light curve with the pyaneti software. The radial velocity measurements were modelled with both a Gaussian process (GP) regression and the so-called floating chunk offset (FCO) technique to simultaneously model the planetary signal and correlated noise associated with stellar activity. Results. Imaging confirms that K2-216 is a single star. Our analysis discloses that the star is a moderately active K5V star of mass 0.70 ± 0.03 M⊙ and radius 0.72 ± 0.03 R⊙. Planet b is found to have a radius of 1.75−0.10+0.17 R⊕ and a 2.17-day orbit in agreement with previous results. We find consistent results for the planet mass from both models: Mp ≈ 7.4 ± 2.2 M⊕ from the GP regression and Mp ≈ 8.0 ± 1.6 M⊕ from the FCO technique, which implies that this planet is a super-Earth. The incident stellar flux is 248(−48)(+220) F⊕. Conclusions. The planet parameters put planet b in the middle of, or just below, the gap of the radius distribution of small planets. The density is consistent with a rocky composition of primarily iron and magnesium silicate. In agreement with theoretical predictions, we find that the planet is a remnant core, stripped of its atmosphere, and is one of the largest planets found that has lost its atmosphere.