Bauer, Florian F.

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[["dc.bibliographiccitation.firstpage","A24"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","632"],["dc.contributor.author","Fuhrmeister, B."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Hildebrandt, L."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Schmitt, J. H. M. M."],["dc.contributor.author","Hintz, D."],["dc.contributor.author","Johnson, E. N."],["dc.contributor.author","Sanz-Forcada, J."],["dc.contributor.author","Schöfer, P."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Cortés-Contreras, M."],["dc.contributor.author","Díez-Alonso, E."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Galadí-Enríquez, D."],["dc.contributor.author","Günther, E. W."],["dc.contributor.author","Kaminski, A."],["dc.contributor.author","Kürster, M."],["dc.contributor.author","Lafarga, M."],["dc.contributor.author","Montes, D."],["dc.date.accessioned","2020-04-06T07:56:28Z"],["dc.date.available","2020-04-06T07:56:28Z"],["dc.date.issued","2019-11-01"],["dc.description.abstract","The He I infrared (IR) triplet at 10830 AA is an important activity indicator for the Sun and in solar-type stars, however, it has rarely been studied in relation to M dwarfs to date. In this study, we use the time-averaged spectra of 319 single stars with spectral types ranging from M0.0 V to M9.0 V obtained with the CARMENES high resolution optical and near-infrared spectrograph at Calar Alto to study the properties of the He I IR triplet lines. In quiescence, we find the triplet in absorption with a decrease of the measured pseudo equivalent width (pEW) towards later sub-types. For stars later than M5.0 V, the He I triplet becomes undetectable in our study. This dependence on effective temperature may be related to a change in chromospheric conditions along the M dwarf sequence. When an emission in the triplet is observed, we attribute it to flaring. The absence of emission during quiescence is consistent with line formation by photo-ionisation and recombination, while flare emission may be caused by collisions within dense material. The He I triplet tends to increase in depth according to increasing activity levels, ultimately becoming filled in; however, we do not find a correlation between the pEW(He IR) and X-ray properties. This behaviour may be attributed to the absence of very inactive stars ($L_{\\rm X}/L_{\\rm bol}$ < -5.5) in our sample or to the complex behaviour with regard to increasing depth and filling in."],["dc.identifier.arxiv","1911.00246v1"],["dc.identifier.doi","10.1051/0004-6361/201936193"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/63790"],["dc.relation.issn","0004-6361"],["dc.relation.issn","1432-0746"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.title.subtitle","The He I triplet at 10830 Å across the M dwarf sequence"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

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