J/A+A/676/A98ivo://CDS.VizieR/J/A+A/676/A98doi:10.26093/cds/vizier/bc-n4/ljiCDSShagatova N.Skopal A.Kundra E.Komzik R.Shugarov S.Y.Pribulla T.,Krushevska V.2026-07-01T14:00:47Z2023-11-16T09:23:48ZCDS support team

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

cds-question@unistra.frlate-type-starsgiant-starsradial-velocityvisible-astronomyNon-dusty late-type giants without a corona and large-scale pulsations represent objects that do not fulfil the conditions under which standard mass-loss mechanisms can be applied efficiently. Despite the progress during the past decades, the driving mechanism of their winds is still unknown. One of the crucial constraints of aspiring wind-driving theories can be provided by the measured velocity and density fields of outflowing matter. The main goal of this work is to match the radial velocities of absorbing matter with a depth in the red giant (RG) atmosphere in the S-type symbiotic star EG And. We measured fluxes and radial velocities of ten FeI absorption lines from spectroscopic observations with a resolution of ~30000. At selected orbital phases, we modelled their broadened profiles, including all significant broadening mechanisms. The selected Fe I absorption lines at 5151-6469{AA} originate at a radial distance ~1.03RG radii from its centre. The corresponding radial velocity is typically ~1km/s, which represents a few percent of the terminal velocity of the RG wind. The high scatter of the radial velocities of several km/s in the narrow layer of the stellar atmosphere points to the complex nature of the near-surface wind mass flow. The average rotational velocity of 11km/s implies that the rotation of the donor star can contribute to observed focusing the wind towards the orbital plane. The orbital variability of the absorbed flux indicates the highest column densities of the wind in the area between the binary components, even though the absorbing neutral material is geometrically more extended from the opposite side of the giant. This wind density asymmetry in the orbital plane region can be ascribed to gravitational focusing by the white dwarf companion. Our results suggest that both gravitational and rotational focusing contribute to the observed enhancement of the RG wind towards the orbital plane, which makes mass transfer by the stellar wind highly efficient.2023A&A...676A..98Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/676/A98CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/676/A98https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/676/A98http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/676/A98https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/676/A98https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/676/A98http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/676/A98GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/676/A98/tablea1Radial velocities of ten FeI absorption lines from our 53 spectra (Sect. 3.1)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julain datedtime.epochdoubleObs.dateObservation date (UT, YYYY/MM/DD.ddd)time.epoch;obsnullablePhaseOrbital phase according to Eq. (1) of the papertime.phasefloatRV5151FeI 5151{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5340FeI 5340{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5371FeI 5371{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5406FeI 5406{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5430FeI 5430{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5435FeI 5435{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5501FeI 5501{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV5507FeI 5507{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV6412FeI 6412{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleRV6469FeI 6469{AA} absorption line radial velocitykm/sphys.veloc;pos.heliocentricdoubleJ/A+A/676/A98/tablea2Absorbed fluxes of ten FeI absorption lines from our 53 spectra (Sect. 3.1)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian datedtime.epochdoubleObs.dateObservation date (UT, YYYY/MM/DD.ddd)time.epoch;obsnullablePhaseOrbital phase according to Eq. (1) of the papertime.phasefloatF5151FeI 5151{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5340FeI 5340{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5371FeI 5371{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5406FeI 5406{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5430FeI 5430{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5435FeI 5435{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5501FeI 5501{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF5507FeI 5507{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF6412FeI 6412{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloatF6469FeI 6469{AA} absorption line absorbed flux1e-15W.m**-2phot.flux;spect.linefloat