EGU21-9861, updated on 04 Mar 2021
https://doi.org/10.5194/egusphere-egu21-9861
EGU General Assembly 2021
© Author(s) 2021. This work is distributed under
the Creative Commons Attribution 4.0 License.

Spectral evolution of Alfvénic turbulence

Roland Grappin1, Andrea Verdini2,3, and Wolf-Christian Müller4
Roland Grappin et al.
  • 1Ecole Polytechnique, LPP, Palaiseau, France (roland.grappin@obspm.fr)
  • 2Università di Firenze, Dipartimento di Fisica e Astronomia, Firenze, Italy
  • 3INAF, OAA, Firenze, Italy
  • 4Technische Universität Berlin, Zentrum für Astronomie und Astrophysik, Hardenbergstr. 36A, 10623 Berlin, Germany

Alfvénic turbulence denotes a regime of MHD turbulence in which Alfvén waves propagating in a given direction along the mean field are dominant, as commonly found in polar regions/coronal holes/fast solar wind. 

Generalization to Alfvénic turbulence of the Iroshnikov-Kraichnan (IK) weak theory concluded that one should observe a time increase of the imbalance between both Alfvén species and observe the so-called “spectral pinning”, i.e., steep spectra (with spectral index m+>3/2) for the dominant energy E+ and flat spectra (with index m-<3/2) for the sub-dominant energy E-.

Since then, observations in the inner heliosphere have shown on the contrary a decrease of imbalance with time, with both species showing the same flat spectra (m± → -3/2) when imbalance is large.

We show here using direct MHD simulations that both behaviors may occur, the control parameters being the solar wind expansion rate as well as initial conditions of the plasma close to the Sun.

How to cite: Grappin, R., Verdini, A., and Müller, W.-C.: Spectral evolution of Alfvénic turbulence, EGU General Assembly 2021, online, 19–30 Apr 2021, EGU21-9861, https://doi.org/10.5194/egusphere-egu21-9861, 2021.

Display materials

Display file

Comments on the display material

to access the discussion