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Issue A&A
Volume 472, Number 3, September IV 2007
Page(s) L51 - L54
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20077936



A&A 472, L51-L54 (2007)
DOI: 10.1051/0004-6361:20077936

Letter

Spicule emission profiles observed in He I 10 830 Å

B. Sánchez-Andrade Nuño1, 2, R. Centeno3, 4, K. G. Puschmann2, J. Trujillo Bueno2, 3, 5, J. Blanco Rodríguez2, and F. Kneer2

1  Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany
2  Institut für Astrophysik, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
    e-mail: bruno@astro.physik.uni-goettingen.de
3  Instituto de Astrofísica de Canarias, C/ Vía Láctea, s/n, 38205 La Laguna, Tenerife, Spain
4  High Altitude Observatory (NCAR), 3080 Center Green Dr. (CG-1), Boulder 80301 CO, USA
5  Consejo Superior de Investigaciones Científicas, Spain

(Received 24 May 2007 / Accepted 25 July 2007)

Abstract
Aims.Off-the-limb observations with high spatial and spectral resolution will help us understand the physical properties of spicules in the solar chromosphere.
Methods.Spectropolarimetric observations of spicules in the He I 10 830 Å multiplet were obtained with the Tenerife Infrared Polarimeter on the German Vacuum Tower Telescope at the Observatorio del Teide (Tenerife, Spain). The analysis shows the variation of the off-limb emission profiles as a function of the distance to the visible solar limb. The ratio between the intensities of the blue and the red components of this triplet $({\cal R}=I_{\rm blue}/I_{\rm red})$ is an observational signature of the optical thickness along the light path, which is related to the intensity of the coronal irradiation.
Results.We present observations of the intensity profiles of spicules above a quiet Sun region. The observable ${\cal R}$ as a function of the distance to the visible limb is also given. We have compared our observational results to the intensity ratio obtained from detailed radiative transfer calculations in semi-empirical models of the solar atmosphere assuming spherical geometry. The agreement is purely qualitative. We argue that future models of the solar chromosphere and transition region should account for the observational constraints presented here.


Key words: Sun: chromosphere -- line: profiles -- techniques: spectroscopic -- instrumentation: spectrographs



© ESO 2007

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