Por favor, use este identificador para citar o enlazar este ítem: http://hdl.handle.net/20.500.12666/334
Título : The CARMENES search for exoplanets around M dwarfs The He I triplet at 10830 Å across the M dwarf sequence
Autor : Fuhrmeister, B.
Czesla, S.
Hildebrandt, L.
Nagel, E.
Schmitt, H. M. M.
Hintz, D.
Johnson, E. N.
Sanz Forcada, J.
Schöfer, P.
Jeffers, S. V.
Caballero, J. A.
Zechmeister, M.
Reiners, A.
Ribas, I.
Amado, P. J.
Quirrenbach, A.
Bauer, F. F.
Béjar, V. J. S.
Cortés Contreras, M.
Díez Alonso, E.
Dreizler, S.
Galadí Enríquez, D.
Guenther, E. W.
Kaminski, A.
Kürster, M.
Lafarga, M.
Montes, D.
Palabras clave : Stars: activity;Stars: chromospheres;Stars: late type
Fecha de publicación : 25-nov-2019
Editorial : EDP Sciences
DOI: https://doi.org/10.1051/0004-6361/201936193
Versión del Editor: https://www.aanda.org/articles/aa/full_html/2019/12/aa36193-19/aa36193-19.html
Citación : Astronomy and Astrophysics 632: A24(2019)
Resumen : The He I infrared (IR) triplet at 10 830 Å 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 (LX∕Lbol < −5.5) in our sample or to the complex behaviour with regard to increasing depth and filling in.
Descripción : Full Table 2 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr ( or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/632/A24
URI : http://hdl.handle.net/20.500.12666/334
E-ISSN : 1432-0746
ISSN : 0004-6361
Aparece en las colecciones: (CAB) Artículos

Ficheros en este ítem:
Fichero Descripción Tamaño Formato  
aa36193-19.pdf1,33 MBAdobe PDFVista previa

Este ítem está sujeto a una licencia Creative Commons Licencia Creative Commons Creative Commons