2008/06/27 by J. M. Borrero, S. K. Solanki · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Field strength #Magnetic field #Magnetic flux #Magnetic reconnection #Penumbra #Physics #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #Sunspot #astro-ph
paper · pdf · doi:10.1086/591220
10 pages, 11 figures (3 color figures, f2,f3,f5,f10,f11 low resolution). Accepted for publication in ApJ. To appear in issue 1, vol 686, October 2008
arxiv created 2008/06/27 · openalex publication_date 2008/10/24 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The vertical stratification of the magnetic field strength in sunspot penumbrae is investigated by means of spectropolarimetric observations at high spatial resolution from the Hinode spacecraft. Assuming that the magnetic field changes linearly with optical depth we find that, in those regions where the magnetic field is more inclined and the Evershed flow is strongest (penumbral intraspines), the magnetic field can either increase or decrease with depth. Allowing more degrees of freedom to the magnetic field stratification reveals that the magnetic field initially decreases from log τ 5 = − 3 until log τ 5 ≃ − 1.0, but increases again below that. The presence of strong magnetic fields near the continuum is at odds with the existence of regions void of magnetic fields at, or right below, the τ 5 = 1 level in the penumbra. However, they are compatible with the presence of a horizontal flux-tube-like field embedded in a magnetic atmosphere.