Volume 445, Number 2, January II 2006
|Page(s)||735 - 745|
|Published online||16 December 2005|
Sensitivity of solar off-limb line profiles to electron density stratification and the velocity distribution anisotropy
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strae 2, 37191 Katlenburg-Lindau, Germany e-mail: email@example.com
2 National Solar Observatory, 950 North Cherry Avenue, Tucson, AZ 85726, USA e-mail: firstname.lastname@example.org
Accepted: 10 September 2005
The effect of the electron density stratification on the intensity profiles of the Ly-α line and the and doublets formed in solar coronal holes is investigated. We employ an analytical 2-D model of the large scale coronal magnetic field that provides a good representation of the corona at the minimum of solar activity. We use the mass-flux conservation equation to determine the outflow speed of the solar wind at any location in the solar corona and take into account the integration along the line of sight (LOS). The main assumption we make is that no anisotropy in the kinetic temperature of the coronal species is considered. We find that at distances greater than 1 from the solar surface the widths of the emitted lines of and are sensitive to the details of the adopted electron density stratification. However, Ly-α, which is a pure radiative line, is hardly affected. The calculated total intensities of Ly-α and the doublet depend to a lesser degree on the density stratification and are comparable to the observed ones for most of the considered density models. The widths of the observed profiles of Ly-α and are well reproduced by most of the considered electron density stratifications, while for the doublet only few stratifications give satisfying results. The densities deduced from SOHO data result in profiles whose widths and intensity ratio are relatively close to the values observed by UVCS although only isotropic velocity distributions are employed. These density profiles also reproduce the other considered observables with good accuracy. Thus the need for a strong anisotropy of the velocity distribution (i.e. a temperature anisotropy) is not so clear cut as previous investigations of UVCS data suggested. However, these results do not rule completely out the existence of some degree of anisotropy in the corona. The results of the present computations also suggest that the data can also be reproduced if protons, heavy ions and electrons have a common temperature, if the hydrogen and heavy-ion spectral lines are also non-thermally broadened by a roughly equal amount.
Key words: Sun: corona / Sun: UV radiation / Sun: solar wind / line: profiles
© ESO, 2005
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