Sökning: WFRF:(Nespral D.) > Super-Earth of 8 Me...
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000 | 05402naa a2200901 4500 | |
001 | oai:research.chalmers.se:97fdb929-51ee-4e14-9317-9bf4a55ebe26 | |
003 | SwePub | |
008 | 181012s2018 | |||||||||||000 ||eng| | |
024 | 7 | a https://doi.org/10.1051/0004-6361/2018328672 DOI |
024 | 7 | a https://research.chalmers.se/publication/5053292 URI |
024 | 7 | a https://research.chalmers.se/publication/5057462 URI |
024 | 7 | a https://research.chalmers.se/publication/5062922 URI |
040 | a (SwePub)cth | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a art2 swepub-publicationtype |
072 | 7 | a ref2 swepub-contenttype |
100 | 1 | a Persson, Carina,d 1964u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)carina64 |
245 | 1 0 | a Super-Earth of 8 Mearth in a 2.2-day orbit around the K5V star K2-216 |
264 | c 2018-10-10 | |
264 | 1 | b EDP Sciences,c 2018 |
338 | a electronic2 rdacarrier | |
520 | a 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. Our aim was to confirm the detection and derive the main physical characteristics of K2-216b, including the mass. We performed a series of follow-up observations: high resolution imaging with the FastCam camera at the TCS, the Infrared Camera and Spectrograph at Subaru, and high resolution spectroscopy with HARPS (ESO, La Silla), HARPS-N (TNG), and FIES (NOT). The stellar spectra were analyzed with the SpecMatch-Emp and SME codes to derive the stellar fundamental 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 floating chunk offset (FCO) technique to simultaneously model the planetary signal and correlated noise associated with stellar activity. 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 Msun and radius 0.72+/-0.03 Rsun. Planet b is found to have a radius of 1.75+0.17-0.10 Rearth and a 2.17-day orbit in agreement with previous results. We find consistent results for the planet mass from both models: 7.4+/-2.2 Mearth from the GP regression, and 8.0+/-1.6 Mearth from the FCO technique, which implies that this planet is a super-Earth. 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. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
653 | a Stars: individual: K2-216 | |
653 | a Planets and satellites: Atmospheres | |
653 | a Techniques: photometric | |
653 | a Techniques: radial velocities | |
653 | a Planetary systems | |
653 | a Planets and satellites: composition | |
700 | 1 | a Fridlund, Malcolm,d 1952u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)malfri |
700 | 1 | a Barragan, O.4 aut |
700 | 1 | a Dai, F.4 aut |
700 | 1 | a Gandolfi, D.4 aut |
700 | 1 | a Hatzes, A. P.4 aut |
700 | 1 | a Hirano, T.4 aut |
700 | 1 | a Grziwa, S.4 aut |
700 | 1 | a Korth, J.4 aut |
700 | 1 | a Prieto-Arranz, J.4 aut |
700 | 1 | a Fossati, L.4 aut |
700 | 1 | a Van Eylen, V.4 aut |
700 | 1 | a Justesen, A. Bo4 aut |
700 | 1 | a Livingston, J.4 aut |
700 | 1 | a Kubyshkina, D.4 aut |
700 | 1 | a Deeg, H. J.4 aut |
700 | 1 | a Guenther, E. W.4 aut |
700 | 1 | a Nowak, G.4 aut |
700 | 1 | a Cabrera, J.4 aut |
700 | 1 | a Eigmüller, Ph4 aut |
700 | 1 | a Csizmadia, Sz.4 aut |
700 | 1 | a Smith, A. M. S.4 aut |
700 | 1 | a Erikson, A.4 aut |
700 | 1 | a Albrecht, S.4 aut |
700 | 1 | a Alonso, R.4 aut |
700 | 1 | a Cochran, W. D.4 aut |
700 | 1 | a Endl, M.4 aut |
700 | 1 | a Esposito, M.4 aut |
700 | 1 | a Fukui, A.4 aut |
700 | 1 | a Heeren, P.4 aut |
700 | 1 | a Hidalgo, D.4 aut |
700 | 1 | a Hjorth, M.4 aut |
700 | 1 | a Kuzuhara, M.4 aut |
700 | 1 | a Narita, N.4 aut |
700 | 1 | a Nespral, D.4 aut |
700 | 1 | a Palle, E.4 aut |
700 | 1 | a Pätzold, M.4 aut |
700 | 1 | a Rauer, H.4 aut |
700 | 1 | a Rodler, F.4 aut |
700 | 1 | a Winn, J. N.4 aut |
710 | 2 | a Chalmers tekniska högskola4 org |
773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 618:33q 618:33x 0004-6361x 1432-0746 |
856 | 4 | u https://research.chalmers.se/publication/506292/file/506292_Fulltext.pdfx primaryx freey FULLTEXT |
856 | 4 | u https://www.aanda.org/articles/aa/pdf/2018/10/aa32867-18.pdf |
856 | 4 8 | u https://doi.org/10.1051/0004-6361/201832867 |
856 | 4 8 | u https://research.chalmers.se/publication/505329 |
856 | 4 8 | u https://research.chalmers.se/publication/505746 |
856 | 4 8 | u https://research.chalmers.se/publication/506292 |
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