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An Ultra-Short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-Like Companion Around K2-141

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An Ultra-Short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-Like Companion Around K2-141 An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141 The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Malavolta, Luca et al. “An Ultra-Short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-Like Companion Around K2-141.” The Astronomical Journal 155, 3 (February 2018): 107 © 2018 American Astronomical Society As Published http://dx.doi.org/10.3847/1538-3881/AAA5B5 Publisher American Astronomical Society Version Final published version Citable link https://hdl.handle.net/1721.1/121206 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astronomical Journal, 155:107 (13pp), 2018 March https://doi.org/10.3847/1538-3881/aaa5b5 © 2018. The American Astronomical Society. All rights reserved. An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141 Luca Malavolta1,2 , Andrew W. Mayo3,4, Tom Louden5 , Vinesh M. Rajpaul6, Aldo S. Bonomo7 , Lars A. Buchhave4 , Laura Kreidberg3,8 , Martti H. Kristiansen9,10, Mercedes Lopez-Morales3 , Annelies Mortier11 , Andrew Vanderburg3,12,27 , Adrien Coffinet13, David Ehrenreich13 , Christophe Lovis13, Francois Bouchy13, David Charbonneau3 , David R. Ciardi14, Andrew Collier Cameron11 , Rosario Cosentino15, Ian J. M. Crossfield16,17,27, Mario Damasso7, Courtney D. Dressing18 , Xavier Dumusque13 , Mark E. Everett19 , Pedro Figueira20, Aldo F. M. Fiorenzano15, Erica J. Gonzales16,28, Raphaëlle D. Haywood3,27 , Avet Harutyunyan15, Lea Hirsch18 , Steve B. Howell21 , John Asher Johnson3, David W. Latham3 , Eric Lopez22, Michel Mayor13, Giusi Micela23, Emilio Molinari15,24 , Valerio Nascimbeni1,2, Francesco Pepe13, David F. Phillips3, Giampaolo Piotto1,2 , Ken Rice25, Dimitar Sasselov3 , Damien Ségransan13 , Alessandro Sozzetti7 , Stéphane Udry13, and Chris Watson26 1 Dipartimento di Fisica e Astronomia “Galileo Galilei,” Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, Italy; luca.malavolta@unipd,it 2 INAF—Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4 Centre for Star and Planet Formation, Niels Bohr Institute & Natural History Museum, University of Copenhagen, DK-1350 Copenhagen, Denmark 5 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 6 University of Cambridge, Astrophysics Group, Cavendish Laboratory, J. J. Thomson Avenue, Cambridge CB3 0HE, UK 7 INAF—Osservatorio Astrofisico di Torino, via Osservatorio 20, I-10025 Pino Torinese, Italy 8 The Harvard Society of Fellows, 78 Mt. Auburn Street, Cambridge, MA 02138, USA 9 DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark 10 Brorfelde Observatory, Observator Gyldenkernes Vej 7, DK-4340 Tølløse, Denmark 11 Centre for Exoplanet Science, SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK 12 Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USA 13 Observatoire Astronomique de l’Université de Genève, 51 ch. des Maillettes, 1290 Versoix, Switzerland 14 Caltech/IPAC-NExScI, Mail Code 100-22, 1200 East California Boulevard, Pasadena, CA 91125, USA 15 INAF—Fundación Galileo Galilei, Rambla José Ana Fernandez Pérez 7, E-38712 Breña Baja, Spain 16 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA 17 Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 18 Astronomy Department, University of California Berkeley, Berkeley, CA 94720-3411, USA 19 National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA 20 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal 21 NASA Ames Research Center, Moffett Field, CA 94035, USA 22 NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA 23 INAF—Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90124 Palermo, Italy 24 INAF—Osservatorio Astronomico di Cagliari, Via della Scienza 5—I-09047 Selargius (CA), Italy 25 SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH93HJ, UK 26 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK Received 2017 November 20; revised 2018 January 4; accepted 2018 January 5; published 2018 February 9 Abstract Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51±0.05RÅ and a mass of 5.08±0.41MÅ, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios. Key words: planetary systems – planets and satellites: composition – planets and satellites: individual (K2-141b, K2-141c) – planets and satellites: interiors – stars: individual (K2-141) – techniques: photometric – techniques: radial velocities Supporting material: machine-readable table 27 NASA Sagan Fellow. 28 National Science Foundation Graduate Research Fellow. 1 The Astronomical Journal, 155:107 (13pp), 2018 March Malavolta et al. 1. Introduction namely Kepler-10b (Batalha et al. 2011) and Kepler-78b (Sanchis-Ojeda et al. 2013). If USP planets were really The origin of ultra-short period (USP) planets, i.e., planets with lava-ocean worlds, their atmospheres would be likely made periods shorter than one day and radii smaller than 2 R , is still Å of heavy-element vapors with a very low pressure and, being unclear. An early hypothesis suggested that USP planets and small tidally locked, would experience extremely high day-night planets in general were originally Hot Jupiters (HJs) that contrasts (Léger et al. 2011). Consequently, the bottom of the underwent strong photo-evaporation due to the high insolation fl ( secondary eclipse is expected to be about at the same level as ux, e.g., thousands of times that of Earth, Lecavelier des Etangs / ) just before after the primary transit, when only the nightside of et al. 2004 ending up with the complete removal of their gaseous the planet is in view. This seems to be the case with Kepler-78b envelope and their solid core exposed. The paucity of gas giants (Sanchis-Ojeda et al. 2013) and Kepler-10b (Esteves et al. observed in the photo-evaporation desert, i.e., the region around a 2015), even though a non-negligible nightside temperature for star where only solid cores of once-gaseous planets could survive, the latter has been reported by Fogtmann-Schulz et al. (2014). is the most convincing proof of evaporation as a viable process to ( The geometric albedos of both planets could not be well form small planets e.g., Lecavelier Des Etangs 2007;Davis& constrained because of the degeneracy between thermal and Wheatley 2009; Ehrenreich & Désert 2011; Beaugé & Nesvorný fl ) ( ) re ected light in the Kepler bandpass, which could be broken 2013 . In the case of USP planets, Sanchis-Ojeda et al. 2014 also with observations of the occultation and phase curve at IR found an occurrence rate of USP planets similar to that of HJs wavelengths (e.g., Schwartz & Cowan 2015). Noteworthy is using data from the Kepler mission, but recently, thanks to Keck the attempt by Rouan et al. (2011) to use a lava-ocean model to spectroscopy on a magnitude-limited subset of the same sample, ( ) interpret the optical occultation and phase curve of Kepler-10b. Winn et al. 2017 discovered that the metallicity distributions of In this paper, we report on the discovery, characterization, and fi the two populations are signi cantly different, thus rejecting the confirmation of an USP planet, and the discovery and validation idea of a common origin. The same study supports a similar of an outer companion planet with grazing transits around an hypothesis in which the progenitors of USP planets are not the HJs active K4 dwarf, K2-141 (EPIC 246393474),discoveredinthe but the so-called mini-Neptunes, i.e., planets with rocky cores and Campaign 12 data of the K2 mission and then observed with – hydrogen helium envelopes, typically with radii between 1.7 and the high-precision HARPS-N spectrograph for RV confirmation. ∼ 3.9 RÅ and masses lower than 10 MÅ.AnoriginofUSPplanets We tackled the determination of mass and radius of the star, as photo-evaporated mini-Neptunes is also consistent with the which ultimately can affect the planets’ properties, using three lack of planets with radii between 2.2 and 3.8 RÅ with independent methods for the atmospheric parameters and fl incident ux higher than 650 times the solar constant including any additional data available from the literature.
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