2015/03/12 by S. Thonhofer, L. R. Bellot Rubio, Thonhofer, Stefan +7
Physics and Astronomy · #FOS: Physical sciences #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1503.03710
openalex publication_date 2015/03/12 · openalex created_date 2022/10/01 · openalex updated_date 2026/07/28
Magnetic fields are one of the most important drivers of the highly dynamic\nprocesses that occur in the lower solar atmosphere. They span a broad range of\nsizes, from large- and intermediate-scale structures such as sunspots, pores\nand magnetic knots, down to the smallest magnetic elements observable with\ncurrent telescopes. On small scales, magnetic flux tubes are often visible as\nMagnetic Bright Points (MBPs). Apart from simple V/I magnetograms, the most\ncommon method to deduce their magnetic properties is the inversion of\nspectropolarimetric data. Here we employ the SIR code for that purpose. SIR is\na well-established tool that can derive not only the magnetic field vector and\nother atmospheric parameters (e.g., temperature, line-of-sight velocity), but\nalso their stratifications with height, effectively producing 3-dimensional\nmodels of the lower solar atmosphere. In order to enhance the runtime\nperformance and the usability of SIR we parallelized the existing code and\nstandardized the input and output formats. This and other improvements make it\nfeasible to invert extensive high-resolution data sets within a reasonable\namount of computing time. An evaluation of the speedup of the parallel SIR code\nshows a substantial improvement in runtime.\n