J/A+A/713/A210ivo://CDS.VizieR/J/A+A/713/A210CDSSiderud E.Eriksson K.Hoefner S.Ahmad A.2026-09-16T08:46:41Z2026-09-16T09:46:13ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmosphereslate-type-starsvariable-starsm-starsMass loss from asymptotic giant branch (AGB) stars is the result of a complex interplay between pulsation, atmospheric dynamics, dust formation, and radiative acceleration. Pulsation periods are a key input in dynamical atmosphere and wind models, and different prescriptions for assigning periods based on stellar parameters may lead to systematic differences in the predicted wind properties. To better constrain this critical parameter, we investigate how the choice of pulsation period affects the wind properties of dynamical atmosphere and wind models of M-type AGB stars by comparing models based on an empirical period-luminosity (P-L) relation with corresponding ones adopting a period-mean density relation derived from 3D pulsation models. We analyse two grids of DARWIN models covering a range of current stellar masses, luminosities, and effective temperatures. For each grid, pulsation periods are assigned using either the P-L relation or the period-mean density relation, allowing for a direct comparison of the resulting dynamical structures and wind properties for pairs of models differing by period only. Independent of the adopted period prescription, the time-averaged wind properties correlate strongly with L*/M*. The pulsation period affects the atmospheric dynamics through changes in the relative timing of shock propagation and dust formation, affecting both wind formation and the resulting wind properties. Shorter periods favour the onset of a wind, and models differing only in pulsation period can exhibit significantly different wind properties. The period-mean density relation provides a physically motivated alternative to the empirical P-L relation by accounting for stellar parameters beyond luminosity, and enables a more direct comparison between DARWIN models and observed Mira variables.2026A&A...713A.210Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/713/A210CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/713/A210https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/713/A210http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/713/A210https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/713/A210https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/713/A210http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/713/A210GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/713/A210/tablea1Fundamental model parameters and the resulting wind and dust characteristicsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMassCurrent stellar masssolMassphys.massfloatlogLStellar luminositylog(solLum)phys.luminosityfloatTeffEffective temperatureKphys.temperature.effectiveintupPiston velocity amplitudekm/sphys.velocfloatPerPLPulsation period PLdtime.periodintdM/dtPLMass-loss rate PLsolMass/yrphys.mass.lossdoubleuinfPLWind velocity PLkm/sphys.velocfloatagrPLGrain radii PLumphys.size.radiusfloatfSiPLDegree of condensed Si PLstat.fit.paramfloatPerP3DPulsation period P3Ddtime.periodintdM/dtP3DMass-loss rate P3DsolMass/yrphys.mass.lossdoubleuinfP3DWind velocity P3Dkm/sphys.velocfloatagrP3DGrain radii P3Dumphys.size.radiusfloatfSiP3DDegree of condensed Si P3Dstat.fit.paramfloat