Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/26890
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Christiansen, Jessie L. | en_US |
dc.contributor.author | Vanderburg, Andrew | en_US |
dc.contributor.author | Burt, Jennifer | en_US |
dc.contributor.author | Fulton, B. J. | en_US |
dc.contributor.author | Batygin, Konstantin | en_US |
dc.contributor.author | Benneke, Björn | en_US |
dc.contributor.author | Brewer, John M. | en_US |
dc.contributor.author | Charbonneau, David | en_US |
dc.contributor.author | Ciardi, David R. | en_US |
dc.contributor.author | Collier Cameron, Andrew | en_US |
dc.contributor.author | Coughlin, Jeffrey L. | en_US |
dc.contributor.author | Crossfield, Ian J. M. | en_US |
dc.contributor.author | Dressing, Courtney | en_US |
dc.contributor.author | Greene, Thomas P. | en_US |
dc.contributor.author | Howard, Andrew W. | en_US |
dc.contributor.author | Latham, David W. | en_US |
dc.contributor.author | MOLINARI, Emilio Carlo | en_US |
dc.contributor.author | Mortier, Annelies | en_US |
dc.contributor.author | Mullally, Fergal | en_US |
dc.contributor.author | Pepe, Francesco | en_US |
dc.contributor.author | Rice, Ken | en_US |
dc.contributor.author | Sinukoff, Evan | en_US |
dc.contributor.author | SOZZETTI, Alessandro | en_US |
dc.contributor.author | Thompson, Susan E. | en_US |
dc.contributor.author | Udry, Stéphane | en_US |
dc.contributor.author | Vogt, Steven S. | en_US |
dc.contributor.author | Barman, Travis S. | en_US |
dc.contributor.author | Batalha, Natasha E. | en_US |
dc.contributor.author | Bouchy, François | en_US |
dc.contributor.author | Buchhave, Lars A. | en_US |
dc.contributor.author | Butler, R. Paul | en_US |
dc.contributor.author | COSENTINO, Rosario | en_US |
dc.contributor.author | Dupuy, Trent J. | en_US |
dc.contributor.author | Ehrenreich, David | en_US |
dc.contributor.author | Fiorenzano, Aldo | en_US |
dc.contributor.author | Hansen, Brad M. S. | en_US |
dc.contributor.author | Henning, Thomas | en_US |
dc.contributor.author | Hirsch, Lea | en_US |
dc.contributor.author | Holden, Bradford P. | en_US |
dc.contributor.author | Isaacson, Howard T. | en_US |
dc.contributor.author | Johnson, John A. | en_US |
dc.contributor.author | Knutson, Heather A. | en_US |
dc.contributor.author | Kosiarek, Molly | en_US |
dc.contributor.author | López-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 | Petigura, Erik | en_US |
dc.contributor.author | Phillips, David F. | en_US |
dc.contributor.author | Piotto, Giampaolo | en_US |
dc.contributor.author | Rogers, Leslie A. | en_US |
dc.contributor.author | Sasselov, Dimitar | en_US |
dc.contributor.author | Schlieder, Joshua E. | en_US |
dc.contributor.author | Ségransan, Damien | en_US |
dc.contributor.author | Watson, Christopher A. | en_US |
dc.contributor.author | Weiss, Lauren M. | en_US |
dc.date.accessioned | 2020-08-27T13:41:09Z | - |
dc.date.available | 2020-08-27T13:41:09Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-6256 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26890 | - |
dc.description.abstract | HD 3167 is a bright (V = 8.9), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 ± 0.38 {M}<SUB>\oplus </SUB> for HD 3167 b, a hot super-Earth with a likely rocky composition ({ρ }<SUB>b</SUB> = {5.60}<SUB>-1.43</SUB><SUP>+2.15</SUP> g cm<SUP>-3</SUP>), and {9.80}<SUB>-1.24</SUB><SUP>+1.30</SUP> {M}<SUB>\oplus </SUB> for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement ({ρ }<SUB>c</SUB> = {1.97}<SUB>-0.59</SUB><SUP>+0.94</SUP> g cm<SUP>-3</SUP>). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 ± 0.045 d (between planets b and c) and a minimum mass of 6.90 ± 0.71 {M}<SUB>\oplus </SUB>. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.°3 because we do not observe transits of planet d. From 1.°3 to 40°, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40° to 60°, Kozai-Lidov oscillations increase the system’s instability, but it can remain stable for up to 100 Myr. Above 60°, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission. | en_US |
dc.language.iso | eng | en_US |
dc.title | Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-3881/aa832d | en_US |
dc.identifier.scopus | 2-s2.0-85029107435 | en_US |
dc.identifier.isi | 000410575200007 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-3881/aa832d | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 154 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 122 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTRONOMICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017AJ....154..122C | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | 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.grantfulltext | open | - |
item.cerifentitytype | Publications | - |
item.openairetype | Article | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
crisitem.journal.journalissn | 0004-6256 | - |
crisitem.journal.ance | E016224 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.orcid | 0000-0002-1742-7735 | - |
crisitem.author.orcid | 0000-0002-7504-365X | - |
crisitem.author.orcid | 0000-0003-1784-1431 | - |
crisitem.author.orcid | 0000-0002-6492-2085 | - |
crisitem.author.orcid | 0000-0002-9900-4751 | - |
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