Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/28767
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Santerne, A. | en_US |
dc.contributor.author | Brugger, B. | en_US |
dc.contributor.author | Armstrong, D. J. | en_US |
dc.contributor.author | Adibekyan, V. | en_US |
dc.contributor.author | Lillo-Box, J. | en_US |
dc.contributor.author | Gosselin, H. | en_US |
dc.contributor.author | Aguichine, A. | en_US |
dc.contributor.author | Almenara, J. -M. | en_US |
dc.contributor.author | Barrado, D. | en_US |
dc.contributor.author | Barros, S. C. C. | en_US |
dc.contributor.author | Bayliss, D. | en_US |
dc.contributor.author | Boisse, I. | en_US |
dc.contributor.author | BONOMO, ALDO STEFANO | en_US |
dc.contributor.author | Bouchy, F. | en_US |
dc.contributor.author | Brown, D. J. A. | en_US |
dc.contributor.author | Deleuil, M. | en_US |
dc.contributor.author | Delgado Mena, E. | en_US |
dc.contributor.author | Demangeon, O. | en_US |
dc.contributor.author | Díaz, R. F. | en_US |
dc.contributor.author | Doyle, A. | en_US |
dc.contributor.author | Dumusque, X. | en_US |
dc.contributor.author | Faedi, F. | en_US |
dc.contributor.author | Faria, J. P. | en_US |
dc.contributor.author | Figueira, P. | en_US |
dc.contributor.author | Foxell, E. | en_US |
dc.contributor.author | Giles, H. | en_US |
dc.contributor.author | Hébrard, G. | en_US |
dc.contributor.author | Hojjatpanah, S. | en_US |
dc.contributor.author | Hobson, M. | en_US |
dc.contributor.author | Jackman, J. | en_US |
dc.contributor.author | King, G. | en_US |
dc.contributor.author | Kirk, J. | en_US |
dc.contributor.author | Lam, K. W. F. | en_US |
dc.contributor.author | LIGI, ROXANNE | en_US |
dc.contributor.author | Lovis, C. | en_US |
dc.contributor.author | Louden, T. | en_US |
dc.contributor.author | McCormac, J. | en_US |
dc.contributor.author | Mousis, O. | en_US |
dc.contributor.author | Neal, J. J. | en_US |
dc.contributor.author | Osborn, H. P. | en_US |
dc.contributor.author | Pepe, F. | en_US |
dc.contributor.author | Pollacco, D. | en_US |
dc.contributor.author | Santos, N. C. | en_US |
dc.contributor.author | Sousa, S. G. | en_US |
dc.contributor.author | Udry, S. | en_US |
dc.contributor.author | Vigan, A. | en_US |
dc.date.accessioned | 2020-12-09T17:27:37Z | - |
dc.date.available | 2020-12-09T17:27:37Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 2397-3366 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28767 | - |
dc.description.abstract | Earth, Venus, Mars and some extrasolar terrestrial planets<SUP>1</SUP> have a mass and radius that is consistent with a mass fraction of about 30% metallic core and 70% silicate mantle<SUP>2</SUP>. At the inner frontier of the Solar System, Mercury has a completely different composition, with a mass fraction of about 70% metallic core and 30% silicate mantle<SUP>3</SUP>. Several formation or evolution scenarios are proposed to explain this metal-rich composition, such as a giant impact<SUP>4</SUP>, mantle evaporation<SUP>5</SUP> or the depletion of silicate at the inner edge of the protoplanetary disk<SUP>6</SUP>. These scenarios are still strongly debated. Here, we report the discovery of a multiple transiting planetary system (K2-229) in which the inner planet has a radius of 1.165 ± 0.066 Earth radii and a mass of 2.59 ± 0.43 Earth masses. This Earth-sized planet thus has a core-mass fraction that is compatible with that of Mercury, although it was expected to be similar to that of Earth based on host-star chemistry<SUP>7</SUP>. This larger Mercury analogue either formed with a very peculiar composition or has evolved, for example, by losing part of its mantle. Further characterization of Mercury-like exoplanets such as K2-229 b will help to put the detailed in situ observations of Mercury (with MESSENGER and BepiColombo<SUP>8</SUP>) into the global context of the formation and evolution of solar and extrasolar terrestrial planets. | en_US |
dc.language.iso | eng | en_US |
dc.title | An Earth-sized exoplanet with a Mercury-like composition | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1038/s41550-018-0420-5 | en_US |
dc.identifier.scopus | 2-s2.0-85046361600 | en_US |
dc.identifier.isi | 000434351700019 | en_US |
dc.identifier.url | https://www.nature.com/articles/s41550-018-0420-5 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 2 | en_US |
dc.relation.firstpage | 393 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | NATURE ASTRONOMY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018NatAs...2..393S | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare 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.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 2397-3366 | - |
crisitem.journal.ance | E240167 | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0002-6177-198X | - |
crisitem.author.orcid | 0000-0002-6257-6051 | - |
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File | Descrizione | Dimensioni | Formato | |
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Santerneetal_2018.pdf | postprint | 4.43 MB | Adobe PDF | Visualizza/apri |
Nat. Astr. main s41550-018-0420-5.pdf | [Administrators only] | 4.73 MB | Adobe PDF |
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