Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/23556
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Dressing, Courtney D. | en_US |
dc.contributor.author | Charbonneau, David | en_US |
dc.contributor.author | Dumusque, Xavier | en_US |
dc.contributor.author | Gettel, Sara | en_US |
dc.contributor.author | Pepe, Francesco | en_US |
dc.contributor.author | Collier Cameron, Andrew | en_US |
dc.contributor.author | Latham, David W. | en_US |
dc.contributor.author | MOLINARI, Emilio Carlo | en_US |
dc.contributor.author | Udry, Stéphane | en_US |
dc.contributor.author | AFFER, Laura | en_US |
dc.contributor.author | BONOMO, ALDO STEFANO | en_US |
dc.contributor.author | Buchhave, Lars A. | en_US |
dc.contributor.author | COSENTINO, Rosario | en_US |
dc.contributor.author | Figueira, Pedro | en_US |
dc.contributor.author | Fiorenzano, Aldo F. M. | en_US |
dc.contributor.author | HARUTYUNYAN, AVET | en_US |
dc.contributor.author | Haywood, Raphaëlle D. | en_US |
dc.contributor.author | Johnson, John Asher | en_US |
dc.contributor.author | Lopez-Morales, Mercedes | en_US |
dc.contributor.author | Lovis, Christophe | en_US |
dc.contributor.author | Malavolta, Luca | en_US |
dc.contributor.author | Mayor, Michel | en_US |
dc.contributor.author | MICELA, Giuseppina | en_US |
dc.contributor.author | Motalebi, Fatemeh | en_US |
dc.contributor.author | NASCIMBENI, VALERIO | en_US |
dc.contributor.author | Phillips, David F. | en_US |
dc.contributor.author | Piotto, Giampaolo | en_US |
dc.contributor.author | Pollacco, Don | en_US |
dc.contributor.author | Queloz, Didier | en_US |
dc.contributor.author | Rice, Ken | en_US |
dc.contributor.author | Sasselov, Dimitar | en_US |
dc.contributor.author | Ségransan, Damien | en_US |
dc.contributor.author | SOZZETTI, Alessandro | en_US |
dc.contributor.author | Szentgyorgyi, Andrew | en_US |
dc.contributor.author | Watson, Chris | en_US |
dc.date.accessioned | 2020-03-25T16:15:51Z | - |
dc.date.available | 2020-03-25T16:15:51Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23556 | - |
dc.description | The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen's University Belfast, and University of Edinburgh. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 313014 (ETAEARTH). C.D. is supported by a National Science Foundation Graduate Research Fellowship. X.D. would like to thank the Swiss National Science Foundation (SNSF) for its support through an Early Postdoc Mobility fellowship. P.F. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through Investigador FCT contracts of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program “Programa Operacional de Factores de Competitividade - COMPETE.” This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. | - |
dc.description.abstract | Kepler-93b is a 1.478 ± 0.019 R_⊕ planet with a 4.7 day period around a bright (V = 10.2), astroseismically characterized host star with a mass of 0.911 ± 0.033 M_☉ and a radius of 0.919 ± 0.011 R_☉. Based on 86 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 32 archival Keck/HIRES observations, we present a precise mass estimate of 4.02 ± 0.68 M _⊕. The corresponding high density of 6.88 ± 1.18 g cm^-3 is consistent with a rocky composition of primarily iron and magnesium silicate. We compare Kepler-93b to other dense planets with well-constrained parameters and find that between 1 and 6 M _⊕, all dense planets including the Earth and Venus are well-described by the same fixed ratio of iron to magnesium silicate. There are as of yet no examples of such planets with masses >6 M _⊕. All known planets in this mass regime have lower densities requiring significant fractions of volatiles or H/He gas. We also constrain the mass and period of the outer companion in the Kepler-93 system from the long-term radial velocity trend and archival adaptive optics images. As the sample of dense planets with well-constrained masses and radii continues to grow, we will be able to test whether the fixed compositional model found for the seven dense planets considered in this paper extends to the full population of 1-6 M _⊕ planets. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Mass of Kepler-93b and The Composition of Terrestrial Planets | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1088/0004-637X/800/2/135 | en_US |
dc.identifier.scopus | 2-s2.0-84924273193 | en_US |
dc.identifier.isi | 000349782500058 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.1088/0004-637X/800/2/135 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 800 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 135 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 35 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | ESP | en_US |
dc.contributor.country | DNK | en_US |
dc.contributor.country | PRT | en_US |
dc.contributor.country | CHE | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015ApJ...800..135D | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.orcid | 0000-0002-1742-7735 | - |
crisitem.author.orcid | 0000-0001-5600-3778 | - |
crisitem.author.orcid | 0000-0002-6177-198X | - |
crisitem.author.orcid | 0000-0002-6492-2085 | - |
crisitem.author.orcid | 0000-0002-9900-4751 | - |
crisitem.author.orcid | 0000-0001-9770-1214 | - |
crisitem.author.orcid | 0000-0002-7504-365X | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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Dressing_2015_ApJ_800_135.pdf | PDF editoriale | 558.71 kB | Adobe PDF | View/Open |
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