Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30734
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Mulders, Gijs D. | en_US |
dc.contributor.author | Pascucci, Ilaria | en_US |
dc.contributor.author | Apai, Dániel | en_US |
dc.contributor.author | FRASCA, Antonio | en_US |
dc.contributor.author | Molenda-Żakowicz, Joanna | en_US |
dc.date.accessioned | 2021-04-12T10:36:58Z | - |
dc.date.available | 2021-04-12T10:36:58Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-6256 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30734 | - |
dc.description.abstract | Host star metallicity provides a measure of the conditions in protoplanetary disks at the time of planet formation. Using a sample of over 20,000 Kepler stars with spectroscopic metallicities from the LAMOST survey, we explore how the exoplanet population depends on host star metallicity as a function of orbital period and planet size. We find that exoplanets with orbital periods less than 10 days are preferentially found around metal-rich stars ([Fe/H] ≃ 0.15 ± 0.05 dex). The occurrence rates of these hot exoplanets increases to ∼30% for super-solar metallicity stars from ∼10% for stars with a sub-solar metallicity. Cooler exoplanets, which reside at longer orbital periods and constitute the bulk of the exoplanet population with an occurrence rate of ≳90%, have host star metallicities consistent with solar. At short orbital periods, P\lt 10 days, the difference in host star metallicity is largest for hot rocky planets (\lt 1.7 {R}\oplus ), where the metallicity difference is [Fe/H] ≃ 0.25 ± 0.07 dex. The excess of hot rocky planets around metal-rich stars implies they either share a formation mechanism with hot Jupiters, or trace a planet trap at the protoplanetary disk inner edge, which is metallicity dependent. We do not find statistically significant evidence for a previously identified trend that small planets toward the habitable zone are preferentially found around low-metallicity stars. Refuting or confirming this trend requires a larger sample of spectroscopic metallicities. | en_US |
dc.language.iso | eng | en_US |
dc.title | A SUPER-SOLAR METALLICITY FOR STARS WITH HOT ROCKY EXOPLANETS | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0004-6256/152/6/187 | en_US |
dc.identifier.scopus | 2-s2.0-85009152620 | en_US |
dc.identifier.isi | 000389057100005 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-6256/152/6/187 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 152 | en_US |
dc.relation.issue | 6 | en_US |
dc.relation.firstpage | 187 | en_US |
dc.relation.numberofpages | 8 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 5 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | POL | 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 | 2016AJ....152..187M | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | 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.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.orcid | 0000-0002-0474-0896 | - |
crisitem.journal.journalissn | 0004-6256 | - |
crisitem.journal.ance | E016224 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Mulders_etal2016.pdf | Mulders et al. 2016, AJ 152, 187 | 2.02 MB | Adobe PDF | View/Open |
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