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

Published online by Cambridge University Press:  24 July 2015

Stefan Thonhofer ,
Luis R. Bellot Rubio ,
Dominik Utz ,
Arnold Hanslmeier  and
Jan Jurçák
Stefan Thonhofer
Affiliation:
Institute of Physics, University of Graz Universitätsplatz 5, A-8010 Graz, Austria email: [email protected] Instituto de Astrofísica de Andalucía, CSIC Glorieta de la Astronomía s/n, E-18008 Granada, Spain
Luis R. Bellot Rubio
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC Glorieta de la Astronomía s/n, E-18008 Granada, Spain
Dominik Utz
Affiliation:
Institute of Physics, University of Graz Universitätsplatz 5, A-8010 Graz, Austria email: [email protected] Instituto de Astrofísica de Andalucía, CSIC Glorieta de la Astronomía s/n, E-18008 Granada, Spain
Arnold Hanslmeier
Affiliation:
Institute of Physics, University of Graz Universitätsplatz 5, A-8010 Graz, Austria email: [email protected]
Jan Jurçák
Affiliation:
Astronomical Institute of the Academy of Sciences Friçova 298, CZ-25165 Ondřejov, Czech Republic
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Abstract

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Magnetic fields are one of the most important drivers of the highly dynamic processes that occur in the lower solar atmosphere. They span a broad range of sizes, from large- and intermediate-scale structures such as sunspots, pores and magnetic knots, down to the smallest magnetic elements observable with current telescopes. On small scales, magnetic flux tubes are often visible as Magnetic Bright Points (MBPs). Apart from simple V/I magnetograms, the most common method to deduce their magnetic properties is the inversion of spectropolarimetric data. Here we employ the SIR code for that purpose. SIR is a well-established tool that can derive not only the magnetic field vector and other atmospheric parameters (e.g., temperature, line-of-sight velocity), but also their stratifications with height, effectively producing 3-dimensional models of the lower solar atmosphere. In order to enhance the runtime performance and the usability of SIR we parallelized the existing code and standardized the input and output formats. This and other improvements make it feasible to invert extensive high-resolution data sets within a reasonable amount of computing time. An evaluation of the speedup of the parallel SIR code shows a substantial improvement in runtime.

Keywords

Sun: photospheretechniques: polarimetricmethods: data analysismethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Symposium S305: Polarimetry: From the Sun to Stars and Stellar Environments , December 2014 , pp. 251 - 256
Copyright
Copyright © International Astronomical Union 2015 

References

Bellot Rubio, L. R. 2003a, in: Trujillo Bueno, J. & Sánchez Almeida, J. (eds.), The Fine Structure of the Penumbra: from Observations to Realistic Physical Models, Proc. Solar Polarization 307 (ASP-CS), p. 301Google Scholar
Bellot Rubio, L. R. 2003b, SIR user's guide, Kiepenheuer Institut für Sonnenphysik, Freiburg, GermanyGoogle Scholar
Pence, W. D., Chiappetti, L., Page, C. G., Shaw, R. A., & Stobie, E. 2010, A&A 524, AA42 Google Scholar
Ruiz Cobo, B. & del Toro Iniesta, J. C. 1992, ApJ 398, 375 CrossRefGoogle Scholar
Schüssler, M., Shelyag, S., Berdyugina, S., Vögler, A., & Solanki, S. K. 2003, ApJ (Letters) 597, L173 CrossRefGoogle Scholar
Steiner, O., Hauschildt, P. H., & Bruls, J. 2001, A&A 372, L13 Google Scholar