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Solar Physics

, 293:10 | Cite as

On the Statistical Properties of Turbulent Energy Transfer Rate in the Inner Heliosphere

  • Luca Sorriso-Valvo
  • Francesco Carbone
  • Silvia Perri
  • Antonella Greco
  • Raffaele Marino
  • Roberto Bruno
Article

Abstract

The transfer of energy from large to small scales in solar wind turbulence is an important ingredient of the long-standing question of the mechanism of the interplanetary plasma heating. Previous studies have shown that magnetohydrodynamic (MHD) turbulence is statistically compatible with the observed solar wind heating as it expands in the heliosphere. However, in order to understand which processes contribute to the plasma heating, it is necessary to have a local description of the energy flux across scales. To this aim, it is customary to use indicators such as the magnetic field partial variance of increments (PVI), which is associated with the local, relative, scale-dependent magnetic energy. A more complete evaluation of the energy transfer should also include other terms, related to velocity and cross-helicity. This is achieved here by introducing a proxy for the local, scale-dependent turbulent energy transfer rate \(\epsilon_{\Delta t}(t)\), based on the third-order moment scaling law for MHD turbulence. Data from Helios 2 are used to determine the statistical properties of such a proxy in comparison with the magnetic and velocity fields PVI, and the correlation with local solar wind heating is computed. PVI and \(\epsilon_{\Delta t}(t)\) are generally well correlated; however, \(\epsilon_{\Delta t}(t)\) is a very sensitive proxy that can exhibit large amplitude values, both positive and negative, even for low amplitude peaks in the PVI. Furthermore, \(\epsilon_{\Delta t}(t)\) is very well correlated with local increases of the temperature when large amplitude bursts of energy transfer are localized, thus suggesting an important role played by this proxy in the study of plasma energy dissipation.

Keywords

Solar wind Turbulence Intermittency 

Notes

Acknowledgements

SP acknowledges support by the Agenzia Spaziale Italiana under the contract ASI-INAF 2015-039-R.O “Missione M4 di ESA: Partecipazione Italiana alla fase di assessment della missione THOR”. RM acknowledges financial support from the program PALSE (Programme Avenir Lyon Saint-Etienne) of the University of Lyon, in the frame of the program Investissements d’Avenir (No. ANR-11-IDEX-0007). The authors declare they have no conflict of interest arising from the above funding.

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Copyright information

© Springer Science+Business Media B.V., part of Springer Nature 2018

Authors and Affiliations

  1. 1.Nanotec – UOS di CosenzaCNRRendeItaly
  2. 2.IIA – U.O.S. di CosenzaCNRRendeItaly
  3. 3.Dipartimento di FisicaUniversità della CalabriaRende (CS)Italy
  4. 4.Laboratoire de Mécanique des Fluides et d’Acoustique, École Centrale de LyonCNRS – Université de LyonÉcullyFrance
  5. 5.IAPS-INAFRomaItaly

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