A quantitative method to optimise magnetic field line fitting of observed coronal loops

L Carcedo; DS Brown; Alan William Hood; Thomas Neukirch; T Wiegelmann

doi:10.1023/B:SOLA.0000013045.65499.da

A quantitative method to optimise magnetic field line fitting of observed coronal loops

L Carcedo, DS Brown, Alan William Hood, Thomas Neukirch, T Wiegelmann

Applied Mathematics

Research output: Contribution to journal › Article › peer-review

Abstract

Many authors use magnetic-field models to extrapolate the field in the solar corona from magnetic data in the photosphere. The accuracy of such extrapolations is usually judged qualitatively by eye, where a less judgemental quantitative approach would be more desirable. In this paper, a robust method for obtaining the best fit between a theoretical magnetic field and intensity observations of coronal loops on the solar disk will be presented. The method will be applied to Yohkoh data using a linear force-free field as an illustration. Any other theoretical model for the magnetic field can be used, provided there is enough freedom in the model to optimize the fit.

Original language	English
Pages (from-to)	29-40
Number of pages	12
Journal	Solar Physics
Volume	218
DOIs	https://doi.org/10.1023/B:SOLA.0000013045.65499.da
Publication status	Published - Dec 2003

Keywords

FORCE-FREE FIELDS
GREENS-FUNCTION METHOD
ACTIVE-REGION LOOPS
NON-CONSTANT-ALPHA
EMISSION-LINE
EXTRAPOLATION
RECONSTRUCTION
MAGNETOGRAMS
POLARIZATION
OSCILLATIONS

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10.1023/B:SOLA.0000013045.65499.da

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title = "A quantitative method to optimise magnetic field line fitting of observed coronal loops",

abstract = "Many authors use magnetic-field models to extrapolate the field in the solar corona from magnetic data in the photosphere. The accuracy of such extrapolations is usually judged qualitatively by eye, where a less judgemental quantitative approach would be more desirable. In this paper, a robust method for obtaining the best fit between a theoretical magnetic field and intensity observations of coronal loops on the solar disk will be presented. The method will be applied to Yohkoh data using a linear force-free field as an illustration. Any other theoretical model for the magnetic field can be used, provided there is enough freedom in the model to optimize the fit.",

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author = "L Carcedo and DS Brown and Hood, {Alan William} and Thomas Neukirch and T Wiegelmann",

year = "2003",

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doi = "10.1023/B:SOLA.0000013045.65499.da",

language = "English",

volume = "218",

pages = "29--40",

journal = "Solar Physics",

issn = "0038-0938",

publisher = "Springer",

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TY - JOUR

T1 - A quantitative method to optimise magnetic field line fitting of observed coronal loops

AU - Carcedo, L

AU - Brown, DS

AU - Hood, Alan William

AU - Neukirch, Thomas

AU - Wiegelmann, T

PY - 2003/12

Y1 - 2003/12

N2 - Many authors use magnetic-field models to extrapolate the field in the solar corona from magnetic data in the photosphere. The accuracy of such extrapolations is usually judged qualitatively by eye, where a less judgemental quantitative approach would be more desirable. In this paper, a robust method for obtaining the best fit between a theoretical magnetic field and intensity observations of coronal loops on the solar disk will be presented. The method will be applied to Yohkoh data using a linear force-free field as an illustration. Any other theoretical model for the magnetic field can be used, provided there is enough freedom in the model to optimize the fit.

AB - Many authors use magnetic-field models to extrapolate the field in the solar corona from magnetic data in the photosphere. The accuracy of such extrapolations is usually judged qualitatively by eye, where a less judgemental quantitative approach would be more desirable. In this paper, a robust method for obtaining the best fit between a theoretical magnetic field and intensity observations of coronal loops on the solar disk will be presented. The method will be applied to Yohkoh data using a linear force-free field as an illustration. Any other theoretical model for the magnetic field can be used, provided there is enough freedom in the model to optimize the fit.

KW - FORCE-FREE FIELDS

KW - GREENS-FUNCTION METHOD

KW - ACTIVE-REGION LOOPS

KW - NON-CONSTANT-ALPHA

KW - EMISSION-LINE

KW - EXTRAPOLATION

KW - RECONSTRUCTION

KW - MAGNETOGRAMS

KW - POLARIZATION

KW - OSCILLATIONS

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U2 - 10.1023/B:SOLA.0000013045.65499.da

DO - 10.1023/B:SOLA.0000013045.65499.da

M3 - Article

SN - 0038-0938

VL - 218

SP - 29

EP - 40

JO - Solar Physics

JF - Solar Physics

ER -

A quantitative method to optimise magnetic field line fitting of observed coronal loops

Abstract

Keywords

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