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dc.contributor.authorBozhinova, I.
dc.contributor.authorHelling, Christiane
dc.contributor.authorScholz, A.
dc.identifier.citationBozhinova , I , Helling , C & Scholz , A 2015 , ' Planetary host stars : evaluating uncertainties in cool model atmospheres ' , Monthly Notices of the Royal Astronomical Society , vol. 450 , no. 1 , pp. 160-182 .
dc.identifier.otherPURE: 194132529
dc.identifier.otherPURE UUID: 41fc41c6-76f5-4d27-b79f-675148d5bfcb
dc.identifier.otherBibCode: 2015MNRAS.450..160B
dc.identifier.otherScopus: 84929833871
dc.identifier.otherWOS: 000356311600010
dc.descriptionChH highlights financial support of the European Community under the FP7 by an ERC starting grant. IB thanks the Physics Trust of the University of St Andrews for supporting her summer placement.en
dc.description.abstractM-dwarfs are emerging in the literature as promising targets for detecting low-mass, Earth-like planets. An important step in this process is to determine the stellar parameters of the M-dwarf host star as accurately as possible. Different well-tested stellar model atmosphere simulations from different groups are widely applied to undertake this task. This paper provides a comparison of different model atmosphere families to allow a better estimate of systematic errors on host-star stellar parameter introduced by the use of one specific model atmosphere family only. We present a comparison of the ATLAS9, MARCS, PHOENIX and DRIFT-PHOENIX model atmosphere families including the M-dwarf parameter space (Teff = 2500-4000 K, log(g) = 3.0-5.0, [M/H] = -2.5to0.5). We examine the differences in the (Tgas, pgas)-structures, in synthetic photometric fluxes and in colour indices. Model atmospheres results for higher log(g) deviate considerably less between different models families than those for lower log(g) for all Teff = 2500-4000 K examined. We compiled the broad-band synthetic photometric fluxes for all available model atmospheres (incl. M-dwarfs and brown dwarfs) for the UKIRT WFCAM ZYJHK, 2MASS JHKs and Johnson UBVRI filters, and calculated related colour indices. Synthetic colours in the IR wavelengths diverge by no more than 0.15 dex amongst all model families. For all spectral bands considered, model discrepancies in colour diminish for higher Teff atmosphere simulations. We notice differences in synthetic colours between all model families and observed example data (including Kepler 42 and GJ1214).
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en
dc.subjectStars: atmospheresen
dc.subjectBrown dwarfsen
dc.subjectStars: late-typeen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titlePlanetary host stars : evaluating uncertainties in cool model atmospheresen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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