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| Titel |
From 1AU solar wind turbulence backward to coronal turbulence: an inverse problem |
| VerfasserIn |
Yue Dong, Andrea Verdini, Roland Grappin |
| Konferenz |
EGU General Assembly 2013
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| Medientyp |
Artikel
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| Sprache |
Englisch
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| Digitales Dokument |
PDF |
| Erschienen |
In: GRA - Volume 15 (2013) |
| Datensatznummer |
250074625
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| Zusammenfassung |
| This work deals with the formation of the low-frequency spectrum of solar wind turbulence,
including the so-called inertial range and the lower frequency 1/f range. Much is known on
the turbulent state of the solar wind plasma at distances larger than 0.3 AU, but few is known
on the turbulent state of the plasma at the sources of the wind, like the coronal plasma.
Characterizing the turbulence state of plasma in the solar corona is thus an inverse
problem.
To solve this inverse problem, we use the MHD expanding box model, which consists in
incorporating in the MHD equations the effects of expansion on a turbulent plasma volume
advected by a wind with constant (radial) velocity, by using comobile coordinates. In spite of
its limitations (assumption of constant expansion), the model includes the basic
effects of expansion (i) anisotropic damping of velocity and magnetic field (ii)
weakening of nonlinear coupling in the perpendicular directions. The code allows in
particular to follow the 3D turbulent evolution of the kinetic and magnetic energy
spectra.
We present here for the first time numerical solutions of the expanding 3D MHD
equations by starting with different initial conditions: we follow the turbulent evolution of the
plasma box imbedded in a radial wind up to 1 AU and compare the final turbulent state with
observations, thus allowing us to determine which initial conditions are acceptable. We vary
three kinds of initial parameters: (1) spectral/components anisotropy (2) Alfvén
species imbalance (3) kinetic/magnetic imbalance. The connection of the results
with available models of the formation of coronal turbulence is discussed at the
end. |
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