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Solar Surface Convection.

Åke Nordlund1, Robert F Stein2, Martin Asplund3

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Solar convection drives surface phenomena and impacts helioseismology. Advanced models accurately simulate these processes, revealing insights into solar abundances and magnetic field structures.

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Area of Science:

  • Solar Physics
  • Plasma Physics
  • Astrophysics

Background:

  • Solar convection is crucial for energy transport and atmospheric dynamics.
  • Observational constraints from spectral lines and flow topology inform models.
  • Previous studies often relied on micro/macroturbulence parameters.

Approach:

  • Reviewing observable properties of solar convection at the surface.
  • Analyzing supercomputer models of radiative-hydrodynamics.
  • Comparing model predictions with detailed spectral line observations.

Key Points:

  • Convection properties at granular scales are well-constrained by observations and models.
  • Mass conservation influences larger-scale convective flows.
  • Convection shapes magnetic field patterns and influences solar abundances.
  • Solar convection is vital for helioseismology, affecting wave excitation and propagation.

Conclusions:

  • Current models accurately reproduce solar surface convection, validating their use.
  • Convective velocities explain spectral line profiles without turbulence parameters.
  • Revised solar abundances have significant implications for helioseismology.
  • Near-surface convection drives atmospheric heating and influences magnetic structures.