Imaging Spectropolarimetry with IBIS II: on the fine structure of G-band bright features

TL;DR

This study uses high-resolution spectropolarimetric observations to analyze the relationship between magnetic fields and brightness in G-band features, revealing that brighter features have higher magnetic filling factors and suggesting sub-arcsecond structures.

Contribution

First spectropolarimetric analysis of quiet Sun G-band features linking brightness to magnetic filling factors at high spatial resolution.

Findings

Brighter G-band features correlate with higher magnetic filling factors.

Filling factors up to 35% are observed in the brightest features.

Large G-band bright features may be clusters of sub-arcsecond bright points.

Abstract

We present new results from first observations of the quiet solar photosphere performed through the Interferometric BIdimensional Spectrometer (IBIS) in spectropolarimetric mode. IBIS allowed us to measure the four Stokes parameters in the FeI 630.15 nm and FeI 630.25 nm lines with high spatial and spectral resolutions for 53 minutes; the polarimetric sensitivity achieved by the instrument is 0.003 the continuum intensity level. We focus on the correlation which emerges between G-band bright feature brightness and magnetic filling factor of ~ 1000 G (kG) fields derived by inverting Stokes I and V profiles. More in detail, we present the correlation first in a pixel-by-pixel study of an approximatively 3 arcsec wide bright feature (a small network patch) and then we show that such a result can be extended to all the bright features found in the dataset at any instant of the time sequence. The higher the kG filling factor associated to a feature the higher the brightness of the feature itself. Filling factors up to about 35 % are obtained for the brightest features. Considering the values of the filling factors derived from the inversion analysis of spectropolarimetric data and the brightness variation observed in G-band data we put forward an upper limit for the smallest scale over which magnetic flux concentrations in intergranular lanes produce a G-band brightness enhancement (~ 0.1''). Moreover, the brightness saturation observed for feature sizes comparable to the resolution of the observations is compatible with large G-band bright features being clusters of sub-arcsecond bright points. This conclusion deserves to be confirmed by forthcoming spectropolarimetric observations at higher spatial resolution.