The Continuum Contrast of Magnetic Elements as a Function of Magnetic Field (Disk Center): Early Studies and Hinode/SP Results

Details The Continuum Contrast of Magnetic Elements as a Function of Magnetic Field (Disk Center): Early Studies and Hinode/SP Results The Continuum Contrast of Magnetic Elements as a Function of Magnetic Field (Disk Center): Early Studies and Hinode/SP Results

Apr 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aspc..437..297k&link_type=abstract

Solar Polarization 6. Proceedings of a conference held in Maui, Hawaii, USA on May 30 to June 4, 2010. Edited by J. R. Kuhn, D.

Astronomy and Astrophysics

Astronomy

Scientific paper

To deepen our understanding of the role of small-scale magnetic fields on the solar irradiance, it is essential to quantify the continuum contrast of magnetic elements in the quiet Sun (QS) network and in active region (AR) plage. By using Hinode/SP disk center data at constant spatial resolution, we aimed at updating results of earlier ground-based studies of contrast vs. magnetogram signal, and to look for systematic differences between AR plages and QS network. We performed a pixel-per-pixel study of continuum contrast vs. longitudinal flux density over large fields of view in AR and in QS (as in earlier studies). Even at Hinode's resolution, the contrast of magnetic elements reaches larger values in the QS than in ARs. We show that this difference cannot be explained by different inclinations of magnetic elements in ARs and QS. We compared our contrast vs. magnetic flux density with earlier studies and attributed the differences both to our proper removal of the pores and their surrounding diffraction-spread radiation, as well as to our enhanced spatial resolution and quasi-absence of scattered light. At Hinode's resolution, the contrast of magnetic elements peaks on average at similar magnetic flux densities in ARs and in the QS, which indicates that the brightest flux tubes have similar sizes in ARs and QS.

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