Helioseismology of sunspots: Confronting observations with three-dimensional MHD simulations of wave propagation

R. Cameron, Laurent Gizon, T. L. Duvall

Research output: Contribution to journalArticle

Abstract

The propagation of solar waves through the sunspot of AR9787 is observed by using temporal cross-correlations of SOHO/MDI Dopplergrams. We then use three-dimensional MHD numerical simulations to compute the propagation of wave packets through self-similar magnetohydrostatic sunspot models. The simulations are set up in such a way as to allow a comparison with observed cross-covariances (except in the immediate vicinity of the sunspot). We find that the simulation and the f-mode observations are in good agreement when the model sunspot has a peak field strength of 3 kG at the photosphere and less so for lower field strengths. Constraining the sunspot model with helioseismology is only possible because the direct effect of the magnetic field on the waves has been fully taken into account. Our work shows that the full-waveform modeling of sunspots is feasible.

Original languageEnglish (US)
Pages (from-to)291-308
Number of pages18
JournalSolar Physics
Volume251
Issue number1-2
DOIs
StatePublished - Sep 1 2008

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helioseismology
sunspots
sunspot
wave propagation
simulation
field strength
magnetohydrostatics
propagation
photosphere
wave packets
cross correlation
waveforms
magnetic field
magnetic fields
modeling

Keywords

  • Sun: helioseismology
  • Sun: magnetic fields
  • Sun: sunspots

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Helioseismology of sunspots : Confronting observations with three-dimensional MHD simulations of wave propagation. / Cameron, R.; Gizon, Laurent; Duvall, T. L.

In: Solar Physics, Vol. 251, No. 1-2, 01.09.2008, p. 291-308.

Research output: Contribution to journalArticle

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N2 - The propagation of solar waves through the sunspot of AR9787 is observed by using temporal cross-correlations of SOHO/MDI Dopplergrams. We then use three-dimensional MHD numerical simulations to compute the propagation of wave packets through self-similar magnetohydrostatic sunspot models. The simulations are set up in such a way as to allow a comparison with observed cross-covariances (except in the immediate vicinity of the sunspot). We find that the simulation and the f-mode observations are in good agreement when the model sunspot has a peak field strength of 3 kG at the photosphere and less so for lower field strengths. Constraining the sunspot model with helioseismology is only possible because the direct effect of the magnetic field on the waves has been fully taken into account. Our work shows that the full-waveform modeling of sunspots is feasible.

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