EGU21-8898
https://doi.org/10.5194/egusphere-egu21-8898
EGU General Assembly 2021
© Author(s) 2021. This work is distributed under
the Creative Commons Attribution 4.0 License.

Turbulent energy transfer in bidimensional numerical models of plasma

Rocio Manobanda1, Christian Vasconez2, Denise Perrone3, Raffaele Marino4, Dimitri Laveder5, Francesco Valentini6, Sergio Servidio6, Pablo Minini7, and Luca Sorriso-Valvo8,9
Rocio Manobanda et al.
  • 1Facultad de Ingenierıa en Sistemas, Electronica e Industrial, Universidad Tecnica de Ambato, Ambato, Ecuador (elimanobanda19@gmail.com)
  • 2Departamento de Fisica, Escuela Politecnica Nacional, Quito, Ecuador
  • 3ASI – Italian Space Agency, Rome, Italy
  • 4Laboratoire de Mecanique des Fluides et d’Acoustique, CNRS, Ecole Centrale de Lyon, Universite Claude Bernard Lyon 1, Ecully, France
  • 5Universite Cote d’Azur, CNRS, Observatoire de la Cote d’Azur, Laboratoire J. L. Lagrange, Nice Cedex 4, France
  • 6Dipartimento di Fisica, Universita della Calabria, Rende, Italy
  • 7Departamento de Fisica, Universidad de Buenos Aires and IFIBA, CONICET, Buenos Aires, Argentina
  • 8Istituto per la Scienza e Tecnologia dei Plasmi (ISTP), Consiglio Nazionale delle Ricerche, Bari, Italy
  • 9Swedish Institute of Space Physics, Angstrom Laboratory, Uppsala, Sweden

Structured, highly variable and virtually collision-free. Space plasma is an unique laboratory for studying the transfer of energy in a highly turbulent environment. This turbulent medium plays an important role in various aspects of the Solar--Wind generation, particles acceleration and heating, and even in the propagation of cosmic rays. Moreover, the Solar Wind continuous expansion develops a strong turbulent character, which evolves towards a state that resembles the well-known hydrodynamic turbulence (Bruno and Carbone). This turbulence is then dissipated from magnetohydrodynamic (MHD) through kinetic scales by different -not yet well understood- mechanisms. In the MHD approach, Kolmogorov-like behaviour is supported by power-law spectra and intermittency measured in observations of magnetic and velocity fluctuations. In this regime, the intermittent cross-scale energy transfer has been extensively described by the Politano--Pouquet (global) law, which is based on conservation laws of the MHD invariants, and was recently expanded to take into account the physics at the bottom of the inertial (or Hall) range, e.g. (Ferrand et al., 2019). Following the 'Turbulence Dissipation Challenge', we study the properties of the turbulent energy transfer using three different bi-dimensional numerical models of space plasma. The models, Hall-MHD (HMHD), Landau Fluid (LF) and Hybrid Vlasov-Maxwell (HVM), were ran in collisionless-plasma conditions, with an out-of-plane ambient magnetic field, and with magnetic diffusivity carefully calibrated in the fluid models. As each model has its own range of validity, it allows us to explore a long-enough range of scales at a period of maximal turbulence activity. Here, we estimate the local and global scaling properties of different energy channels using a, recently introduced, proxy of the local turbulent energy transfer (LET) rate (Sorriso-Valvo et al., 2018). This study provides information on the structure of the energy fluxes that transfers (and dissipates) most of the energy at small scales throughout the turbulent cascade. 

How to cite: Manobanda, R., Vasconez, C., Perrone, D., Marino, R., Laveder, D., Valentini, F., Servidio, S., Minini, P., and Sorriso-Valvo, L.: Turbulent energy transfer in bidimensional numerical models of plasma, EGU General Assembly 2021, online, 19–30 Apr 2021, EGU21-8898, https://doi.org/10.5194/egusphere-egu21-8898, 2021.

Corresponding presentation materials formerly uploaded have been withdrawn.