| Issue |
A&A
Volume 566, June 2014
|
|
|---|---|---|
| Article Number | A46 | |
| Number of page(s) | 12 | |
| Section | The Sun | |
| DOI | https://doi.org/10.1051/0004-6361/201322903 | |
| Published online | 09 June 2014 | |
The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet⋆
1 Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
e-mail: dorozco@iac.es
2 Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
3 Consejo Superior de Investigaciones Científicas, 28037 Madrid, Spain
Received: 23 October 2013
Accepted: 28 March 2014
Context. Determining the magnetic field vector in quiescent solar prominences is possible by interpreting the Hanle and Zeeman effects in spectral lines. However, observational measurements are scarce and lack high spatial resolution.
Aims. We determine the magnetic field vector configuration along a quiescent solar prominence by interpreting spectropolarimetric measurements in the He i 1083.0 nm triplet obtained with the Tenerife Infrared Polarimeter installed at the German Vacuum Tower Telescope of the Observatorio del Teide.
Methods. The He i 1083.0 nm triplet Stokes profiles were analyzed with an inversion code that takes the physics responsible for the polarization signals in this triplet into account. The results are put into a solar context with the help of extreme ultraviolet observations taken with the Solar Dynamic Observatory and the Solar Terrestrial Relations Observatory satellites.
Results. For the most probable magnetic field vector configuration, the analysis depicts a mean field strength of 7 gauss. We do not find local variations in the field strength except that the field is, on average, lower in the prominence body than in the prominence feet, where the field strength reaches ~25 gauss. The averaged magnetic field inclination with respect to the local vertical is ~77°. The acute angle of the magnetic field vector with the prominence main axis is 24° for the sinistral chirality case and 58° for the dextral chirality. These inferences are in rough agreement with previous results obtained from the analysis of data acquired with lower spatial resolutions.
Key words: Sun: chromosphere / Sun: filaments, prominences
A movie is available in electronic form at http://www.aanda.org
© ESO, 2014
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