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Magnetic fields are one of the most important drivers of the highly dynamicprocesses that occur in the lower solar atmosphere. They span a broad range ofsizes, from large- and intermediate-scale structures such as sunspots, poresand magnetic knots, down to the smallest magnetic elements observable withcurrent telescopes. On small scales, magnetic flux tubes are often visible asMagnetic Bright Points (MBPs). Apart from simple $V/I$ magnetograms, the mostcommon method to deduce their magnetic properties is the inversion ofspectropolarimetric data. Here we employ the SIR code for that purpose. SIR isa well-established tool that can derive not only the magnetic field vector andother atmospheric parameters (e.g., temperature, line-of-sight velocity), butalso their stratifications with height, effectively producing 3-dimensionalmodels of the lower solar atmosphere. In order to enhance the runtimeperformance and the usability of SIR we parallelized the existing code andstandardized the input and output formats. This and other improvements make itfeasible to invert extensive high-resolution data sets within a reasonableamount of computing time. An evaluation of the speedup of the parallel SIR codeshows a substantial improvement in runtime.

Parallelization of the SIR code for the investigation of small-scale features in the solar photosphere