Inferring the magnetic field vector in the quiet Sun

Abstract

In the past, spectropolarimetric data from Hinode/SP has been employed to infer the distribution of the magnetic field vector in the quiet Sun. While some authors have found predominantly horizontal magnetic fields, others favor an isotropic distribution. In this paper, we investigate whether it is actually possible to accurately retrieve the magnetic field vector in regions with very low polarization signals (e.g: internetwork), employing the \ion{Fe}{I} line pair at 6300 {\AA}. We first perform inversions of the Stokes vector observed with Hinode/SP in the quiet Sun at disk center in order to confirm the distributions retrieved by other authors. We then carry out several Monte-Carlo simulations with synthetic data where we show that the observed distribution of the magnetic field vector can be explained in terms of purely vertical ($\gamma=0\deg$) and weak fields ($\bar{B}<20$ G), that are misinterpreted by the analysis technique (Stokes inversion code) as being horizontal ($\gamma \approx 90\deg$) and stronger ($\bar{B} \approx 100$ G), due to the effect of the photon noise. This casts doubts as to whether previous results, presenting the distributions for the magnetic field vector peaking at $\gamma=90\deg$ and $\bar{B}=100$ G, are actually correct. We propose that an accurate determination of the magnetic field vector can be achieved by decreasing the photon noise to a point where most of the observed profiles posses Stokes $Q$ or $U$ profiles that are above the noise level. Unfortunately, for noise levels as low as $2.8\times 10^{-4}$ only 30% of the observed region with Hinode/SP have strong enough $Q$ or $U$ signals, implying that the magnetic field vector remains unknown in the rest of the internetwork.