Volume 509, January 2010
|Number of page(s)||9|
|Published online||26 January 2010|
The outer atmospheric layers of the early M dwarf Gliese 1
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg,
Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany e-mail: elexen;email@example.com
2 Interdisziplinäres Zentrum für Wissenschaftliches Rechnen (IWR), Im Neuenheimer Feld 368, 69120 Heidelberg, Germany
3 Steward Observatory, Univ. of Arizona, Tucson, AZ 85721, USA e-mail: firstname.lastname@example.org
4 RSAA, College of Science, The Australian National University, Cotter Road , Weston Creek ACT 2611, Australia e-mail: email@example.com
Accepted: 5 October 2009
Using infrared and high-resolution optical observations of the M dwarf Gliese 1, we investigated the temperatures in the upper atmospheric layers of this star with low atmospheric activity. To fit the H and metal line profiles, the normal radiative equilibrium temperature decrease must be truncated at about log above which a steep chromospheric (T≈ 4900 K) rise must be imposed. Unfortunately, the position of the onset of the chromosphere depends to some extent on the temperature distribution in the inner parts of the photosphere. The chromosphere is just not sufficiently optically thick to be seen in the infrared up to ≈30 μm. The persistent strength of the TiO bands leads us to check for indications of surface inhomogeneities with negative results.
Key words: stars: atmospheres / stars: chromospheres / stars: late-type / stars: low-mass / stars: fundamental parameters
© ESO, 2010
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