The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Optimization of the Spectral Line Inversion Code

被引：87

作者：

Centeno, R. ^{[1
]}

Schou, J. ^{[2
,3
]}

Hayashi, K. ^{[2
]}

Norton, A. ^{[2
]}

Hoeksema, J. T. ^{[2
]}

Liu, Y. ^{[2
]}

Leka, K. D. ^{[4
]}

Barnes, G. ^{[4
]}

机构：

[1] NCAR, High Altitude Observ, Boulder, CO 80301 USA

[2] Stanford Univ, HEPL Solar Phys, Stanford, CA 94305 USA

[3] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany

[4] NwRA, Boulder, CO 80301 USA

来源：

SOLAR PHYSICS | 2014年 / 289卷 / 09期

基金：

美国国家科学基金会;

关键词：

Helioseismic and Magnetic Imager; Solar Dynamics Observatory; Photosphere; Sun; magnetic fields; Techniques; polarimetric; DYNAMICS-OBSERVATORY SDO; STOKES PROFILE ANALYSIS;

D O I：

10.1007/s11207-014-0497-7

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Very Fast Inversion of the Stokes Vector (VFISV) is a Milne-Eddington spectral line inversion code used to determine the magnetic and thermodynamic parameters of the solar photosphere from observations of the Stokes vector in the 6173 Fe i line by the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO). We report on the modifications made to the original VFISV inversion code in order to optimize its operation within the HMI data pipeline and provide the smoothest solution in active regions. The changes either sped up the computation or reduced the frequency with which the algorithm failed to converge to a satisfactory solution. Additionally, coding bugs which were detected and fixed in the original VFISV release are reported here.

引用

页码：3531 / 3547

页数：17

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