Spectral evolution of Alfvénic turbulence

<p>Alfv&#233;nic turbulence denotes a regime of MHD turbulence in which Alfv&#233;n waves propagating in a given direction along the mean field are dominant, as commonly found in polar regions/coronal holes/fast solar wind.<span>&#160;</span></p><p>Generalization to Alfv&#233;nic turbulence of the Iroshnikov-Kraichnan (IK) weak theory concluded that one should observe a time increase of the imbalance between both Alfv&#233;n species and observe the so-called &#8220;spectral pinning&#8221;, 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-.</p><p>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_&#177;&#160;&#8594; -3/2) when imbalance is large.</p><p>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.</p>