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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/28664
Title: K2-291b: A Rocky Super-Earth in a 2.2 day Orbit
Authors: Kosiarek, Molly R.
Blunt, Sarah
López-Morales, Mercedes
Crossfield, Ian J. M.
Sinukoff, Evan
Petigura, Erik A.
Gonzales, Erica J.
PORETTI, Ennio 
Malavolta, Luca 
Howard, Andrew W.
Isaacson, Howard
Haywood, Raphaëlle D.
Ciardi, David R.
Bristow, Makennah
Collier Cameron, Andrew
Charbonneau, David
Dressing, Courtney D.
Figueira, Pedro
Fulton, Benjamin J.
Hardee, Bronwen J.
Hirsch, Lea A.
Latham, David W.
Mortier, Annelies
Nava, Chantanelle
Schlieder, Joshua E.
Vanderburg, Andrew
Weiss, Lauren
BONOMO, ALDO STEFANO 
Bouchy, François
Buchhave, Lars A.
Coffinet, Adrien
Damasso, Mario 
Dumusque, Xavier
Lovis, Christophe
Mayor, Michel
MICELA, Giuseppina 
MOLINARI, Emilio Carlo 
Pepe, Francesco
Phillips, David
Piotto, Giampaolo
Rice, Ken
Sasselov, Dimitar
Ségransan, Damien
SOZZETTI, Alessandro 
Udry, Stéphane
Watson, Chris
Issue Date: 2019
Journal: THE ASTRONOMICAL JOURNAL 
Number: 157
Issue: 3
First Page: 116
Abstract: K2-291 is a solar-type star with a radius of R <SUB>*</SUB> = 0.899 ± 0.034 R <SUB>☉</SUB> and mass of M<SUB>*</SUB> = 0.934 ± 0.038 M <SUB>☉</SUB>. From the K2 C13 data, we found one super-Earth planet (R <SUB> p </SUB> = {1.589}<SUB>-0.072</SUB><SUP>+0.095</SUP> R <SUB>⊕</SUB>) transiting this star on a short period orbit (P = {2.225177}<SUB>-6.8{{e</SUB>}{--}5}<SUP>+6.6{{e</SUP>}{--}5} days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M <SUB> p </SUB> = 6.49 ± 1.16 M <SUB>⊕</SUB>. We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84{}<SUB>-2.03</SUB><SUP>+2.50</SUP> g cm<SUP>-3</SUP>, the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star’s lifetime.
URI: http://hdl.handle.net/20.500.12386/28664
URL: https://iopscience.iop.org/article/10.3847/1538-3881/aafe83
https://arxiv.org/abs/1901.04558
ISSN: 0004-6256
DOI: 10.3847/1538-3881/aafe83
Bibcode ADS: 2019AJ....157..116K
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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