Coronal Heating, Weak MHD Turbulence and Scaling Laws

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dc.creatorRappazzo, A. F.
dc.creatorVelli, M.
dc.creatorEinaudi, G.
dc.creatorDahlburg, R. B.
dc.date2007-01-30
dc.date2007-07-15
dc.date.accessioned2026-07-07T10:36:49Z
dc.date.available2026-07-07T10:36:49Z
dc.descriptionLong-time high-resolution simulations of the dynamics of a coronal loop in cartesian geometry are carried out, within the framework of reduced magnetohydrodynamics (RMHD), to understand coronal heating driven by motion of field lines anchored in the photosphere. We unambiguously identify MHD anisotropic turbulence as the physical mechanism responsible for the transport of energy from the large scales, where energy is injected by photospheric motions, to the small scales, where it is dissipated. As the loop parameters vary different regimes of turbulence develop: strong turbulence is found for weak axial magnetic fields and long loops, leading to Kolmogorov-like spectra in the perpendicular direction, while weaker and weaker regimes (steeper spectral slopes of total energy) are found for strong axial magnetic fields and short loops. As a consequence we predict that the scaling of the heating rate with axial magnetic field intensity $B_0$, which depends on the spectral index of total energy for given loop parameters, must vary from $B_0^{3/2}$ for weak fields to $B_0^{2}$ for strong fields at a given aspect ratio. The predicted heating rate is within the lower range of observed active region and quiet Sun coronal energy losses.
dc.description4 pages, 5 figures, uses emulateapj, complies with published version
dc.identifierhttps://arxiv.org/abs/astro-ph/0701872
dc.identifierhttp://arxiv.org/abs/astro-ph/0701872
dc.identifierAstrophys.J.657:L47-L52,2007
dc.identifierdoi:10.1086/512975
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180181
dc.subjectAstrophysics
dc.subjectPlasma Physics
dc.subjectSpace Physics
dc.titleCoronal Heating, Weak MHD Turbulence and Scaling Laws
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