J/MNRAS/462/1577ivo://CDS.VizieR/J/MNRAS/462/1577doi:10.26093/cds/vizier.74621577CDSYildiz M.Celik Orhan Z.Kayhan C.2024-08-16T20:18:12Z2018-03-22T15:17:56ZCDS support team

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

cds-question@unistra.frlate-type-starsstellar-massesstellar-distanceSo-called scaling relations based on oscillation frequencies have the potential to reveal the mass and radius of solar-like oscillating stars. In the derivation of these relations, it is assumed that the first adiabatic exponent at the surface ({Gamma}_1s_) of such stars is constant. However, by constructing interior models for the mass range 0.8-1.6M_{sun}_, we show that {Gamma}_1s_ is not constant at stellar surfaces for the effective temperature range with which we deal. Furthermore, the well-known relation between large separation and mean density also depends on {Gamma}_1s_. Such knowledge is the basis for our aim of modifying the scaling relations. There are significant differences between masses and radii found from modified and conventional scaling relations. However, a comparison of predictions of these relations with the non-asteroseismic observations of Procyon A reveals that new scaling relations are effective in determining the mass and radius of stars. In the present study, solar-like oscillation frequencies of 89 target stars (mostly Kepler and CoRoT) were analysed. As well as two new reference frequencies ({nu}_min1_ and {nu}_min2_) found in the spacing of solar-like oscillation frequencies of stellar interior models, we also take into account {nu}_min0_. In addition to the frequency of maximum amplitude, these frequencies have a very strong diagnostic potential in the determination of fundamental properties. The present study applies the derived relations from the models to the solar-like oscillating stars, and computes their effective temperatures using purely asteroseismic methods. There are in general very close agreements between effective temperatures from asteroseismic and non-asteroseismic (spectral and photometric) methods. For the Sun and Procyon A, for example, the agreement is almost total.2016MNRAS.462.1577Yhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/462/1577CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/corot : CoRoT observation log (N2-4.4) (CoRoT 2016)V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/462/1577https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/462/1577http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/462/1577https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/462/1577https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/462/1577http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/462/1577GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/462/1577/tablea1 (Basic properties of target stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/462/1577/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/462/1577/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/462/1577/tablea1?GETtext/xml+votable180.050000true292.08265537.05981530.0055555555555555566/14578 14581 14585 14751 14763 14767 14770-14771 14777-14779 14794 14819 14824 14827 14918 14921-14922 14924-14926 14930-14932 14935-14936 14938-14939 14941 14947-14948 14956 14959-14960 14963 14967 14969 14973 15041 15044 15057 15061-15062 15106 15109-15110 15112 15121 15124 15129 15131-15133 15142 15145-15146 15154-15157 15168-15170 15172-15174 15178 22036 22120 22122 22300 23575 30289 30294 30878 33281 45485https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/462/1577?format=asciidefaultJ/MNRAS/462/1577/tablea1Basic properties of target starsSimbadNameSimbad column added by the CDSmeta.idcharnumaxFrequency of maximum amplitudeuHzem.freqfloatRefReferencesmeta.refcharStarStar name (1)meta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_numaxrms uncertainty on numaxuHzstat.errorfloatnumin0? Reference frequencies for min0uHzem.freq;src.varfloatnullablee_numin0? rms uncertainty on numin0uHzstat.errorfloatnullablenumin1? Reference frequencies for min1uHzem.freq;src.varfloatnullablee_numin1? rms uncertainty on numin1uHzstat.errorfloatnullablenumin2? Reference frequencies for min2uHzem.freq;src.varfloatnullablee_numin2? rms uncertainty on numin2uHzstat.errorfloatnullable<Dnu>Mean large separation between oscillation frequenciesuHzpos.angDistance;stat.meanfloate_<Dnu>rms uncertainty on <Dnu>uHzstat.errorfloat<dnu02>? Mean small separation between oscillation frequenciesuHzpos.angDistance;stat.meanfloatnullableTeSEffective temperature from spectra (see Section 2)Kphys.temperature.effectiveinte_TeSrms uncertainty on TeSKstat.errorintTeVK? Effective temperature from V-K colour index (see Section 2)Kphys.temperature.effectiveintnullablee_TeVK? rms uncertainty on TeVKKstat.errorintnullableTeBV? Effective temperature from B-V colour index (see Section 2)Kphys.temperature.effectiveintnullablee_TeBV? rms uncertainty on TeBVKstat.errorintnullableTesis0? Effective temperature from minima min0 (see Section 3)Kphys.temperature.effectiveintnullablee_Tesis0? rms uncertainty on Tesis0Kstat.errorintnullableTesis1? Effective temperature from minima min1 (see Section 3)Kphys.temperature.effectiveintnullablee_Tesis1? rms uncertainty on Tesis1Kstat.errorintnullableTesis2? Effective temperature from minima min2 (see Section 3)Kphys.temperature.effectiveintnullablee_Tesis2? rms uncertainty on Tesis2Kstat.errorintnullableMscaMass from the new scaling relations (see Section 3)solMassphys.massfloate_Mscarms uncertainty on MscasolMassstat.errorfloatM1scaMass from the conventional scaling relations (see Section 3)solMassphys.massfloate_M1scarms uncertainty on M1scasolMassstat.errorfloatMlit? Mass from the literature (see Section 3)solMassphys.massfloatnullablee_Mlit? rms uncertainty on MlitsolMassstat.errorfloatnullableRscaRadius from the new scaling relations (see Section 3)solRadphys.size.radiusfloate_Rscarms uncertainty on RscasolRadstat.errorfloatR1scaRadius from the conventional scaling relations (see Section 3)solRadphys.size.radiusfloate_R1scarms uncertainty on R1scasolRadstat.errorfloatRlit? Radius from the literature (see Section 3)solRadphys.size.radiusfloatnullablee_Rlit? rms uncertainty on RlitsolRadstat.errorfloatnullableloggscaSurface gravity from the new scaling relations (see Section 3)log(cm.s**-2)phys.gravityfloate_loggscarms uncertainty on loggscalog(cm.s**-2)stat.errorfloatlogg1scaSurface gravity from the conventional scaling relations (see Section 3)log(cm.s**-2)phys.gravityfloate_logg1scarms uncertainty on logg1scalog(cm.s**-2)stat.errorfloatloggspc? Surface gravity from spectralog(cm.s**-2)phys.gravityfloatnullablee_loggspc? rms uncertainty on loggspclog(cm.s**-2)stat.errorfloatnullable_RAPsotions from Simbab (right ascension part)degpos.eq.ra;meta.mainnullable_DEPsotions from Simbab (declination part)degpos.eq.dec;meta.mainnullableJ/MNRAS/462/1577/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference numbermeta.id;meta.mainintBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notechar