Abstract
Context. Polar magnetic fields play a key role in the solar magnetic cycle and they are the source of a significant portion of the interplanetary magnetic field. However, observations of the poles are challenging and hence our understanding of the polar magnetic environment is incomplete. Aims. We deduce properties of small-scale magnetic features in the polar region using high-resolution data and specifically aim to determine the flux per patch above which one magnetic polarity starts to dominate over the other. Methods. We study the high spatial resolution, seeing-free observations of the north solar polar region, obtained with the IMaX instrument on-board the balloon-borne SUNRISE observatory during June 2009, at the solar activity minimum. We performed inversions of the full Stokes vector recorded by IMaX to retrieve atmospheric parameters of the Sun’s polar region, mainly the temperature stratification and the magnetic field vector. Results. We infer kilo-Gauss (kG) magnetic fields in patches harbouring polar faculae, without resorting to a magnetic filling factor. Within these patches we find the maxima of the magnetic field to be near the dark narrow lanes, which are shifted towards the disc centre side in comparison to the maxima in continuum intensity. In contrast, we did not find any fields parallel to the solar surface with kG strengths. In addition to the kG patches, we found the polar region to be covered in patches of both polarities, which have a range of sizes. We find the field strength of these patches to increase with increasing size and flux, with the smaller patches showing a significant dispersion in field strength. The dominating polarity of the north pole during this phase of the solar cycle is found to be maintained by the larger patches with fluxes above 2.3 × 1017 Mx.
Highlights
A thorough and coherent investigation of the Sun’s polar magnetic environment is a key element, for a better understanding of fundamental processes in the Sun, such as the solar activity cycle, and for the structure of a significant portion of the interplanetary magnetic field, especially at the minimum of the activity cycle
Tsuneta et al (2008b) investigated the data from SOT spectropolarimeter (SOT/SP) and found patches of unipolar magnetic flux concentrations with field strengths exceeding 1 kG, wherein the magnetic field vector is nearly vertical to the local solar surface
We want to emphasise here that the kG field strengths in the Hinode data are only retrieved after applying a filling factor, whereas the IMaX data deliver these values directly without taking recourse to such a measure
Summary
A thorough and coherent investigation of the Sun’s polar magnetic environment is a key element, for a better understanding of fundamental processes in the Sun, such as the solar activity cycle, and for the structure of a significant portion of the interplanetary magnetic field, especially at the minimum of the activity cycle. The presence of polar faculae harbouring kilo-Gauss (kG) magnetic fields was reported by several authors analysing ground-based observations (Homann et al 1997; Okunev & Kneer 2004; Blanco Rodríguez et al 2007). These studies were based on the inference of the magnetic fields from observations of Stokes I and V of Fraunhofer lines in the visible spectral range. Blanco Rodríguez & Kneer (2010) extended their previous study (Blanco Rodríguez et al 2007) of the polar faculae, analysing the full Stokes vector in the infrared
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