Comptes Rendus
no. 2
Observation and theoretical modeling of electron scale solar wind turbulence
[Observations et modélisation théorique de la turbulence à lʼéchelle électronique dans le vent solaire]
Fouad Sahraoui1  ; Melvyn L. Goldstein2 ; K. Abdul-Kader1 ; Gérard Belmont1 ; Laurence Rezeau1, 3 ; Patrick Robert1 ; Patrick Canu1
1 Laboratoire de Physique des Plasmas, CNRS-École Polytechnique, Observatoire de Saint-Maur, 4, avenue de Nepture, 94107 Saint-Maur-des-Fossés, France
2 NASA Goddard Space Flight Center, Code 673, Greenbelt, MD 20771, USA
3 Université Pierre-et-Marie-Curie, 4, place Jussieu, 75005 Paris, France
Comptes Rendus. Physique, Propagation and plasmas: new challenges, new applications, Volume 12 (2011) no. 2, pp. 132-140.

La turbulence aux échelles magnétohydrodynamique (MHD) dans le vent solaire a été étudiée pendant plus de trois décennies, au moyen dʼanalyses de données, de modélisations théoriques et de simulations numériques. Cependant, les plus petites échelles nʼont pas été explorées jusquʼà très récemment. Ici, nous passons en revue les résultats récents sur la cascade et la dissipation de la turbulence du vent solaire à lʼéchelle des électrons. Grâce aux données à haute résolution temporelle des champs magnétique et électrique des satellites Cluster, nous avons obtenu les spectres de la turbulence jusquʼà 100 Hz (dans le référentiel du satellite) et avons mis en évidence une zone de dissipation dʼénergie autour de la fréquence fρe correspondant à lʼéchelle de giration des électrons. Avant sa dissipation, lʼénergie subit deux cascades : une cascade classique à la Kolmogorov avec une loi dʼéchelle f−1.6 en dessus de lʼéchelle de giration des protons, et une nouvelle cascade en f−2.3 aux échelles sub-protoniques jusquʼà lʼ échelle électronique. Au-dessus fρe le spectre a une loi de puissance plus pentue en f−4.1 jusquʼà la limite dʼobservation donnée par le niveau de bruit de lʼinstrument. La résolution numérique des équations linéaires de Maxwell–Vlasov combinées aux récentes prédictions de la théorique Gyrocinétique, montrent que ces résultats sont conformes à un scénario de cascade quasi-2D suivant le mode dʼAlfvén cinétique (KAW). Une analyse plus récente dʼun autre jeu de données, où les séparations de cluster étaient de ∼200km, nous a permis dʼexplorer les échelles sous-proton en utilisant la technique k-filtering, et de confirmer la nature quasi-2D de la turbulence à ces échelles-là.

Turbulence at MagnetoHydroDynamics (MHD) scales in the solar wind has been studied for more than three decades, using data analysis, theoretical and numerical modeling. However, smaller scales have not been explored until very recently. Here, we review recent results on the first observation of cascade and dissipation of the solar wind turbulence at the electron scales. Thanks to the high resolution magnetic and electric field data of the Cluster spacecraft, we computed the spectra of turbulence up to ∼100Hz (in the spacecraft reference frame) and found evidence of energy dissipation around the Doppler-shifted electron gyroscale fρe. Before its dissipation, the energy is shown to undergo two cascades: a Kolmogorov-like cascade with a scaling f−1.6 above the proton gyroscale, and a new f−2.3 cascade at the sub-proton and electron gyroscales. Above fρe the spectrum has a steeper power law ∼f−4.1 down to the noise level of the instrument. Solving numerically the linear Maxwell–Vlasov equations combined with recent theoretical predictions of the Gyro-Kinetic theory, we show that the present results are consistent with a scenario of a quasi-two-dimensional cascade into Kinetic Alfvén modes (KAW). New analyses of other data sets, where the Cluster separation (of about ∼200km) allowed us to explore the sub-proton scales using the k-filtering technique, and to confirm the 2D nature of the turbulence at those scales.

Publié le :
DOI : 10.1016/j.crhy.2010.11.008
Keywords: Solar wind, Turbulence, Dissipation, Cluster, Heating, k-Filtering
Mots-clés : Vent solaire, Turbulence, Dissipation, Cluster, Chauffage

Fouad Sahraoui 1 ; Melvyn L. Goldstein 2 ; K. Abdul-Kader 1 ; Gérard Belmont 1 ; Laurence Rezeau 1, 3 ; Patrick Robert 1 ; Patrick Canu 1

1 Laboratoire de Physique des Plasmas, CNRS-École Polytechnique, Observatoire de Saint-Maur, 4, avenue de Nepture, 94107 Saint-Maur-des-Fossés, France
2 NASA Goddard Space Flight Center, Code 673, Greenbelt, MD 20771, USA
3 Université Pierre-et-Marie-Curie, 4, place Jussieu, 75005 Paris, France 
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Fouad Sahraoui; Melvyn L. Goldstein; K. Abdul-Kader; Gérard Belmont; Laurence Rezeau; Patrick Robert; Patrick Canu. Observation and theoretical modeling of electron scale solar wind turbulence. Comptes Rendus. Physique, Propagation and plasmas: new challenges, new applications, Volume 12 (2011) no. 2, pp. 132-140. doi : 10.1016/j.crhy.2010.11.008. https://comptes-rendus.academie-sciences.fr/physique/articles/10.1016/j.crhy.2010.11.008/

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