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Inversion of Zeeman Line Profiles Using Central Moments

Published online by Cambridge University Press:  27 June 2012

M. Faurobert ,
C. Fang ,
T. Corbard ,
P. Mein ,
H. Uitenbroek ,
N. Mein ,
V. Bommier  and
M. Faurobert
P. Mein
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC Paris 06, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France
H. Uitenbroek
Affiliation:
National Solar Observatory, operated by the Association of Universities for Research in Astronomy, Inc. (AURA), for the National Science Foundation, Sacramento Peak, PO Box 62, Sunspot, NM 88349, USA
N. Mein
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC Paris 06, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France
V. Bommier
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC Paris 06, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France
M. Faurobert
Affiliation:
UMR 6525 H. Fizeau, Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, Campus Valrose, 06108 Nice, France
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Abstract

A new inversion method derived from central moments of Zeeman line profiles (ICM), is used to determine magnetic field vectors (Mein et al. 2011). Two quantities A1 and A2 combining moments of profiles I ± S (S = Q,U,V) are nearly linear functions of the longitudinal and transverse components and lead to the field components through very fast iterations. Optimized exponents reduce noise effects. The ICM inversion does not require Milne Eddington approximation and can be used in a wide range of solar models.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 55: 4th French-Chinese Meeting on Solar Physics - Understanding Solar Activity: Advances and Challenges , 2012 , pp. 83 - 86
Copyright
© EAS, EDP Sciences 2012

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References

Bommier, V., Landi Degl’Innocenti, E., Landolfi, M., & Molodij, G., 2007, A&A, 464, 323
Mein, P., Uitenbroek, H., Mein, N., Bommier, V., & Faurobert, M., 2011, A&A, 535, A45
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