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

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

Research output: Contribution to journalArticlepeer-review

40 Citations (Scopus)

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 languageEnglish
Pages (from-to)29-40
Number of pages12
JournalSolar Physics
Volume218
DOIs
Publication statusPublished - 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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