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Testing the Steady-State Fluctuation Relation in the Solar Photospheric Convection.

Giorgio Viavattene1, Giuseppe Consolini2, Luca Giovannelli1

  • 1Università degli Studi di Roma "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy.

Entropy (Basel, Switzerland)
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PubMed
Summary

Solar turbulent convection, an irreversible process, exhibits statistical features aligning with the Gallavotti-Cohen steady-state fluctuation theorem. This finding confirms the theorem

Keywords:
Sunastrophysical fluid dynamicsconvectionfluctuation theoremsnon-equilibrium stationary statephotospherespectroscopy

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Area of Science:

  • Solar physics
  • Non-equilibrium thermodynamics
  • Statistical mechanics

Background:

  • Turbulent thermal convection on the Sun is a key non-equilibrium phenomenon.
  • It occurs in a quasi-steady state with continuous entropy production.
  • The Gallavotti-Cohen steady-state fluctuation theorem provides a framework for understanding such systems.

Purpose of the Study:

  • To investigate the statistical features of local entropy production rate in solar quiet regions.
  • To compare these features with the symmetry conjecture of the Gallavotti-Cohen theorem.
  • To determine if solar turbulent convection satisfies the theorem's predictions at a local level.

Main Methods:

  • Analysis of statistical features of a proxy for local entropy production rate.
  • Examination across different timescales in solar quiet regions.
  • Comparison with the Gallavotti-Cohen steady-state fluctuation theorem's symmetry conjecture.

Main Results:

  • The study analyzed statistical properties of solar turbulent convection.
  • A proxy for local entropy production rate was investigated in solar quiet regions.
  • Results demonstrated consistency with the Gallavotti-Cohen theorem's predictions.

Conclusions:

  • Solar turbulent convection locally satisfies the symmetries predicted by the Gallavotti-Cohen steady-state fluctuation theorem.
  • This provides empirical support for the theorem in astrophysical contexts.
  • The findings enhance our understanding of non-equilibrium processes in stars.