2012/11/28 by M. Franz, Morten Franz · 2 citations
Physics and Astronomy · #Electrical and Electromagnetic Research #Inversion (geology) #Magnetic field #Magnetic structure #Photosphere #Polarity (international relations) #Resolution (logic) #Scientific Research and Discoveries #Solar and Space Plasma Dynamics #Spectral line #Sunspot #Surface (topology) #astro-ph.SR
paper · pdf · doi:10.1002/asna.201211789
published in Astronomische Nachrichten 333(10), 1009-1012 (Wiley) · 5 Pages, 2 Figures, 3 Movies To appear in Astronomical Notes Vol 333, Issue 10, pp.1009-1012
arxiv created 2012/11/28 · openalex publication_date 2012/12/01 · arxiv updated 2015/03/12 · openalex created_date 2019/06/27 · openalex updated_date 2026/08/05
Abstract A precise knowledge of the surface structure of sunspots is essential to construct adequate input models for helioseismic inversion tools. We summarize our recent findings about the velocity and magnetic field in and around sunspots using HINODE observation. To this end we quantize the horizontal and vertical component of the penumbral velocity field at different levels of precision and study the moat flow around sunspot. Furthermore, we find that a significant amount of the penumbral magnetic fields return below the surface within the penumbra. Finally, we explain why the related opposite polarity signals remain hidden in magnetograms constructed from measurements with limited spectral resolution (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)