2015/04/15 by D. Orozco Suárez, D. Orozco Suarez, A. Asensio Ramos +1 · 1 citation
Computer Science · Physics and Astronomy · #Astrophysics #Chromosphere #Earth's magnetic field #Geology #Magnetic field #Optics #Physics #Polarimeter #Polarimetry #Solar Radiation and Photovoltaics #Solar and Space Plasma Dynamics #Solar telescope #Sponge spicule #Stellar, planetary, and galactic studies #Sunspot #Telescope #astro-ph.SR
paper · pdf · doi:10.1088/2041-8205/803/2/l18
Published in ApJ Letters
openalex publication_date 2015/04/15 · arxiv created 2015/04/17 · arxiv updated 2015/04/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Proving the magnetic configuration of solar spicules has hitherto been difficult due to the lack of spatial resolution and image stability during off-limb ground-based observations. We report spectropolarimetric observations of spicules taken in the He i 1083 nm spectral region with the Tenerife Infrared Polarimeter II at the German Vacuum Tower Telescope of the Observatorio del Teide (Tenerife, Canary Islands, Spain). The data provide the variation with geometrical height of the Stokes I , Q , U , and V profiles, whose encoded information allows the determination of the magnetic field vector by means of the HAZEL inversion code. The inferred results show that the average magnetic field strength at the base of solar spicules is about 80 gauss, and then it decreases rapidly with height to about 30 gauss at a height of 3000 km above the visible solar surface. Moreover, the magnetic field vector is close to vertical at the base of the chromosphere and has mid-inclinations (about 50°) above 2 Mm height.