Modeling helioseismic modes in the magnetic atmosphere of the Sun

B. Pintér*

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review


The pulsation of the solar surface is caused by acoustic waves traveling in the solar interior. Thorough analyses of observational data indicate that these f and p helioseismic oscillation modes are not bounced back completely at the surface but they partially penetrate into the atmosphere. Atmospheric effects and their possible observational application are investigated in one-dimensional magnetohydrodynamic models. It is found that f and p mode frequencies are shifted of the order of μHz due to the presence of an atmospheric magnetic field. This shift varies with the direction of the wave propagation.Resonant coupling of global helioseismic modes to local Alfvén and slow waves reduce the life time of the global modes. The resulting line width of the frequency line is of the order of nHz, and it also varies with propagation angle. These features enable us to use helioseismic observations in magnetic diagnostics of the lower atmosphere.

Original languageEnglish
Pages (from-to)738-742
Number of pages5
JournalAstronomische Nachrichten
Issue number8
Publication statusPublished - Aug 2007


  • Sun: atmosphere
  • Sun: helioseismology
  • Sun: magnetic fields
  • Sun: oscillations


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