EDP Sciences
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meta n /th c mmt Ptd c mmtc 13 A/images/ac div>/div> <7210-15.htmlame=equiv="content-type"#FN1">⋆ supsd stars from the Herschel MESS sample"> aitle_toc"> <-re Lags" cpterna2"> _content-t-re Lag-1ts.for-url=> or/?dkeyaname="prism.keyword" conten/medin=1 &> uthor_insti Point or_insti Point hor_insti Point thor_insti Point _author_insti Point uthor_insti Point r_insti Point uthor_insti Point _aution_author_insti Point _author_insti Point author_insti Point _insti Point uthor_insti Point on_author_insti Point hor_insti Pointaff" > > h Subscri nu i>ss from ers is a key ingredient for our understanding of many fields of astrophysics, including stellar evolution and the chemical enrichment of the interstellar medium (ISM) via stellar yields. Nevertheless, many questions are still unsolved, one of which is the geometry of the mass-loss process. <i>Aims. <i/>Taking advant p nu i>e resure <i>Herschel <i/>Mass loss itation_onschel MESS stiated a coordinated effort to characterise the geometry of mass loss from evolved red giants at various spatial scales.<i>Methods. <i/>For this p p nu i> used thered interferometric Instrument (MIDI) to resolve the inner envelope of 14 asymptotic giant branch stars (AGBs) in the MESS sample. In this contribution we present an overview of the interferometric data collected within the frame of our Large Programme, and we also add archive data for completeness. We studied the geometry of the inner atmosphere by comparing the observations with predictions from different geometric models.<i>Results. <i/>Asymmetrie p nu i>ected forwing five stars: R Leo, RT Vir, <i>π<i/><sup>1<s/s"/h>Subscrist foe-maπ/sups1 sups/PointSubscrist foe-maN/Point<>such chemistry. We speculate that this fact is related to the characteristics of the dust grains. Except for one star, no interferometric variability is detected, i.e. the changes in size of the shells of non-mira stars correspond to changes of the visibility of less than 10%. The observed spectral variability confirms previous findings from the literature. The detection of dust in our sample follows the location of the AGBs in the IRAS colour–colour diagram: more dust is detect–around oxygen-rich stars in region II and in the carbon stars in region VII. The SiC dust feature does not appear in the visibility spectrum of the U Ant and S Sct, which are two carbon stars with detached shells. This finding has implications for the theory of SiC dust formation."> itle_toc"> nu s"/h>SubscriHomepag o_pub ignrileftn i sups⋆ supsd ign> mefferent geomete Programmeriste Eu ane/h>Organgscolou> iland, 191 Siriphanicht and SSond">rn Hs reth prehysic Gar effort tos 073.D-0711, 076.D-0620, 077.D-0294, 078.D-012y">080.D-0801, 081.D-0021, 083.D-0234, 086.D-0737, 086.D-89a n187.D-0924, 089.D-056y">090.D-410, 091.C-0468, 091.D-0344t p©cationName/Pp c _content-tn i ass="moduletoolbtype Cu0 Brt Inerscmnt="hs6Mbutten> ebutten "moduletoolbty-Item" auth"Abondlights "> ebutten "moduletoolbty-Item" =" spnreRe spn hanights nt="ht-siq">c nt="ht- Onpe="textctp://www.edpscanelts.for-> auth" ep>Cu0 Brt Inerscmnt="hs qhow m.k chalt;icouab16, 7ghtst="Eightt pDLarge of less thanInerscs from t="EDlr/?taften d" c in thcu0 Brt Inerscmnt="hs ing vew Rodul48-96 , Thasaften meta n mp; Astroph. The s updt gradew y feromekadeyst pSubscriber /> - auth" t=textc ep>Icterilctrwnloadms. <int="hs may tak onhed ov p jQuery(function ($) { var soured.png" alt="EDP t" typejs/ nt="ht-tatate" type="appli ions); er div>
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