

Paper: 
MultiLine Determination of the Turbulent Magnetic Field from the Second Solar Spectrum of MgH 
Volume: 
358, Solar Polarization 4 
Page: 
317 
Authors: 
Bommier, V.; Landi Degl'Innocenti, E.; Molodij, G. 
Abstract: 
This paper presents an analysis of the Q_{1,2}(6−12) lines of the Q band of the A^{2}Π–X^{2}Σ^{+} (0,0) transition of MgH, whose linear polarization was measured with THEMIS, on November 21, 2004, in a quiet region of the Sun (North pole), 4″ inside the solar limb. This analysis is performed as follows: a) The Hanle effect parameter, Γ_{H}, is derived by applying the differential Hanle effect method between the two extreme pairs of lines. Assuming no depolarizing collisions, a magnetic field strength follows, which is found to be 9.2 G, in agreement with previous observations of the same kind. b) This Γ_{H} parameter is entered in a code solving the nonLTE polarized radiative transfer equations, and the other depolarizing parameter, namely the depolarizing collision rate, is then derived by adjusting the computed polarization to the observed one. Thus an average value of the rate per colliding hydrogen atom α^{(2)} = 1.20 × 10^{−9} cm^{3} s^{−1} is obtained for the upper levels of the 12 lines (with a standard deviation of 0.21 × 10^{−9} cm^{3} s^{−1}). The corresponding modeldependent depolarizing rate is D^{(2)} = (4.2±0.7) × 10^{7} s^{−1} at h = 200 km. c) This depolarizing rate is now introduced in the conversion of the Γ_{H} parameter in terms of magnetic field strength: an average turbulent field strength of 29 ± 12G is derived as the final value, at a height h = 200 ± 80km where the polarization is formed. The HönlLondon factors of the lines under interest have been recalculated, leading to detect an error of a factor 2 in the recent literature. The derived value B = 29 ± 12G at h = 200 ± 80km is in fairly good agreement with previous determinations based on the interpretation of the Sr I 4607 Å limb polarization, which has led to fields in the range 35–60 G. Given the error bars, it seems unnecessary to put forward different formation regions for the Sr I and MgH lines. This work has been presented in detail by Bommier et al. (2006), under the title “Collisional influence on the differential Hanle effect method applied to the second solar spectrum of the A^{2}Π–X^{2}Σ^{+} (0,0) band of MgH.” 



