J/A+A/580/A27ivo://CDS.VizieR/J/A+A/580/A27doi:10.26093/cds/vizier.35800027CDSMoravveji E.Aerts C.Papics P.I.Triana S.A.Vandoren B.2017-10-12T13:00:22Z2015-07-22T09:36:00ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frb-starsKIC 10526294 is a very slowly rotating and slowly pulsating late B-type star. Its 19 consecutive dipole gravity modes constitute a series with almost constant period spacing. This unique collection of identified modes probes the near-core environment of this star and holds the potential to reveal the size and structure of the overshooting zone on top of the convective core, as well as the mixing properties of the star. We pursue forward seismic modelling based on adiabatic eigenfrequencies of equilibrium models for eight extensive evolutionary grids tuned to KIC 10526294, by varying the initial mass, metallicity, chemical mixture, and the extent of the overshooting layer on top of the convective core. We examine models for both OP and OPAL opacities and test the occurrence of extra diffusive mixing. We find a tight mass, metallicity relation within the ranges M~3.13 to 3.25M_{sun}_ and Z~0.014 to 0.028. We deduce that an exponentially decaying diffusive core overshooting prescription describes the seismic data better than a step function formulation and derive a value of f_ov between 0.017 and 0.018. Moreover, the inclusion of extra diffusive mixing with a value of log D_mix between 1.75 and 2.00dex (with Dmix in cm^2^/sec) improves the goodness-of-fit based on the observed and modelled frequencies with a factor 11 compared to the case where no extra mixing is considered, irrespective of the (M,Z) combination within the allowed seismic range. The inclusion of diffusive mixing in addition to core overshooting is essential to explain the structure in the observed period spacing pattern of this star. Moreover, we deduce that an exponentially decaying prescription for the core overshooting is to be preferred over a step function. Our best models for KIC 10526294 approach the seismic data to a level that they can serve future inversion of its stellar structure.2015A&A...580A..27Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/580/A27CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/580/A27https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/580/A27http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/580/A27https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/580/A27https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/580/A27http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/580/A27GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/580/A27/table3Compilation of best models from different grids (Table 2) and their input parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModel[1/11] Model numbermeta.id;meta.mainintprimaryFSimbad column added by the CDSmeta.ref.urlchardataDownload the corresponding model data filemeta.ref.urlcharGridType of grid usedmeta.id;stat.fitcharOpacityOpacity table used (OP or OPAL)meta.id;stat.fitcharMixtureMixture used (NP12, A09, A05+Ne) (1)meta.id;stat.fitcharMass[3.1/3.5] MasssolMassphys.massfloatXini[0.69/0.71] Initial X abundancephys.abund.XfloatZini[0.01/0.028] Initial Z abundancephys.atmol.initialfloatXc[0.25/0.7] Centre hydrogen abundancephys.abund.Xfloatfov[0/0.21] Overshooting parameter for all models except for Model 10 where we list {alpha}_o_vstat.paramfloatlogDmix[1.75/2]? Extra diffusive mixinglog(cm**2.s**-1)stat.paramfloatnullablechi2r[1711/23200] Reduced {chi}^2^ valuestat.fit.chi2intchi2P[1.4/23] {chi}^2^ value from Papics et al. (2014A&A...570A...8P)stat.fit.chi2floatJ/A+A/580/A27/headHeaders of model filesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModelSimbad column added by the CDSmeta.id;stat.fitintnullabledataDownload the model filemeta.ref.urlcharFileModel file namemeta.id;meta.filecharN[5366/5491] Number of grid pointsmeta.numberintM*Stellar massgphys.massdoubleR*Stellar radiuscmphys.angSize;srcdoubleL*Stellar luminosity (erg/s)1e-07Wphys.luminositydoubleNcol[19] Number of columns in the model filemeta.numberint