A possible signature of terrestrial planet formation in the chemical composition of solar analogs

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dc.contributor.authorRamirez, I
dc.contributor.authorAsplund, Martin
dc.contributor.authorBaumann, P
dc.contributor.authorMelendez, Jorge
dc.contributor.authorBensby, T
dc.date.accessioned2015-12-13T22:44:53Z
dc.date.issued2010
dc.date.updated2016-02-24T09:38:15Z
dc.description.abstractRecent studies have shown that the elemental abundances in the Sun are anomalous when compared to most (about 85%) nearby solar twin stars. Compared to its twins, the Sun exhibits a deficiency of refractory elements (those with condensation temperatures TC ≥ 900≤ K) relative to volatiles (TC ≥ 900≤ K). This finding is speculated to be a signature of the planet formation that occurred more efficiently around the Sun compared with the majority of solar twins. Furthermore, within this scenario, it seems more likely that the abundance patterns found are specifically related to the formation of terrestrial planets. In this work we analyze abundance results from six large independent stellar abundance surveys to determine whether they confirm or reject this observational finding. We show that the elemental abundances derived for solar analogs in these six studies are consistent with the TC trend suggested as a planet formation signature. The same conclusion is reached when those results are averaged heterogeneously. We also investigate the dependency of the abundances with first ionization potential (FIP), which correlates well with TC. A trend with FIP would suggest a different origin for the abundance patterns found, but we show that the correlation with TC is statistically more significant. We encourage similar investigations of metal-rich solar analogs and late F-type dwarf stars, for which the hypothesis of a planet formation signature in the elemental abundances makes very specific predictions. Finally, we examine a recent paper that claims that the abundance patterns of two stars hosting super-Earth like planets contradict the planet formation signature hypothesis. Instead, we find that the chemical compositions of these two stars are fully compatible with our hypothesis.
dc.identifier.issn0004-6361
dc.identifier.urihttp://hdl.handle.net/1885/79510
dc.publisherSpringer
dc.sourceAstronomy and Astrophysics
dc.subjectKeywords: Chemical compositions; Condensation temperature; Different origins; Dwarf stars; Earth-like planets; Elemental abundance; First ionization potentials; Fully compatible; Planet formation; Planetary system; Refractory elements; Stars: abundances; Sun: abund planetary systems; Stars: abundances; Sun: abundances
dc.titleA possible signature of terrestrial planet formation in the chemical composition of solar analogs
dc.typeJournal article
local.bibliographicCitation.issue4
local.bibliographicCitation.startpageA33
local.contributor.affiliationRamirez, I, Max Planck Institute for Astrophysics
local.contributor.affiliationAsplund, Martin, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationBaumann, P, Max-Planck-Institut für Astrophysik
local.contributor.affiliationMelendez, Jorge, Centro de Astrofisica da Universidade do Porto
local.contributor.affiliationBensby, T, European Southern Observatory
local.contributor.authoremailu4042723@anu.edu.au
local.contributor.authoruidAsplund, Martin, u4042723
local.description.embargo2037-12-31
local.description.notesImported from ARIES
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationf5625xPUB7936
local.identifier.citationvolume521
local.identifier.doi10.1051/0004-6361/201014456
local.identifier.scopusID2-s2.0-77958024076
local.identifier.thomsonID000284150900094
local.identifier.uidSubmittedByf5625
local.type.statusPublished Version

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