VFISV: Very Fast Inversion of the Stokes Vector for the Helioseismic and Magnetic Imager

By J. Borrero, S. Tomczyk, M. Kubo, H. Socas-Navarro, J. Schou, S. Couvidat, R. Bogart. 2009

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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.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/987224689720a79fa076efa7161682bdc5acd8e6

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Citations in the corpus

The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance (2014, methodology): “Several changes and optimizations have been introduced in VFISV since its release (Borrero et al., 2011).”
EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION (2011, methodology): “To obtain vector magnetograms, Stokes parameters are first derived from filtergrams observed over a 12-minute interval and then inverted through a Milne-Eddington based algorithm, the Very Fast Inversion of the Stokes Vector (VFISV; Borrero et al. 2011).”
Comparison of Line-of-Sight Magnetograms Taken by the Solar Dynamics Observatory/Helioseismic and Magnetic Imager and Solar and Heliospheric Observatory/Michelson Doppler Imager (2012, methodology): “The Stokes parameters [I, Q, U, V ] are computed from those measurements, and are further inverted (Borrero et al., 2011) and SOLA: hmilosmag_v0315.tex; 16 March 2012; 9:08; p. 2 disambiguated (Metcalf et al., 2006; Leka et al., 2009) to retrieve the vector magnetic field.”
The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs – Space-Weather HMI Active Region Patches (2014, methodology): “The expression relating the final CEA map coordinate [x, y] to the heliographic longitude and latitude [φ, λ] follows Equations (79) and (80) of Calabretta and Greisen (2002), compliant with the World Coordinate System (WCS) standard (e.g. Thompson, 2006).”