Bibcode
Borrero, J. M.; Tomczyk, S.; Kubo, M.; Socas-Navarro, H.; Schou, J.; Couvidat, S.; Bogart, R.
Bibliographical reference
Solar Physics, Volume 273, Issue 1, pp.267-293
Advertised on:
10
2011
Journal
Citations
282
Refereed citations
262
Description
In this paper we describe in detail the implementation and main
properties of a new inversion code for the polarized radiative transfer
equation (VFISV: Very Fast Inversion of the Stokes Vector). VFISV will
routinely analyze pipeline data from the Helioseismic and Magnetic
Imager (HMI) on-board of the Solar Dynamics Observatory (SDO). It will
provide full-disk maps (4096×4096 pixels) of the magnetic field
vector on the Solar Photosphere every ten minutes. For this reason VFISV
is optimized to achieve an inversion speed that will allow it to invert
sixteen million pixels every ten minutes with a modest number (approx.
50) of CPUs. Here we focus on describing a number of important details,
simplifications and tweaks that have allowed us to significantly speed
up the inversion process. We also give details on tests performed with
data from the spectropolarimeter on-board of the Hinode spacecraft.
Related projects
Magnetism, Polarization and Radiative Transfer in Astrophysics
Magnetic fields pervade all astrophysical plasmas and govern most of the variability in the Universe at intermediate time scales. They are present in stars across the whole Hertzsprung-Russell diagram, in galaxies, and even perhaps in the intergalactic medium. Polarized light provides the most reliable source of information at our disposal for the
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