Damping of helioseismic modes in steady state

B. Pintér*, R. Erdélyi, R. New

*Corresponding author for this work

Research output: Contribution to journalLetterpeer-review

12 Citations (SciVal)


The effects of an equilibrium flow in the internal regions of the Sun are studied on the damping of helioseismic f- and p-modes. The Sun is modeled as a multi-layered plasma, where the upper parts, representing the chromosphere and corona, are embedded in a horizontally unidirectional though vertically inhomogeneous magnetic field, while the lower part, representing the sub-photospheric polytropic region, is in a steady equilibrium state. The steady state sub-surface region can be considered as a first approximation of dynamic motions (e.g., differential rotation, sub-surface flows, meridional flows, convective motion, etc.). The frequencies and the line-widths of eigenmodes are affected by sub-surface flow and atmospheric magnetic fields. A key contribution to the effects comes from the universal mechanism of resonant absorption. When both atmospheric magnetic field and sub-surface flows are present, a complex picture of competition between these two effects is found. The theoretically predicted frequency shifts in a steady state show promise of explaining the observed effects. Changes in damping of f- and p-modes caused by changes (e.g. cyclic, if any) of steady state flows are predicted.

Original languageEnglish
Pages (from-to)L17-L20
JournalAstronomy and Astrophysics
Issue number1
Publication statusPublished - 2001


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


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