Parameters and Initial Conditions

  • Victor Montagud-CampsEmail author
Part of the Springer Theses book series (Springer Theses)


We use here EBM simulations to study the generation of the spectral anisotropy in the distance range [0.2,1] AU, which as seen previously (Sect.  4.3.1) is different in the fast and slow wind at 1 AU. Here, we present the initial parameters that will be used to study spectral anisotropy in the expanding solar wind.


  1. 1.
    D’Amicis R, Bruno R (2015) On the origin of highly Alfvénic slow solar wind. Astrophys J 805(1):1–9CrossRefGoogle Scholar
  2. 2.
    Dasso Milano LJ, Matthaeus WH, Smith CW (2005) Anisotropy in fast and slow solar wind fluctuations. Astrophys J 635(2):L181–L184.
  3. 3.
    Oughton S, Matthaeus WH, Smith CW, Breech B, Isenberg P (2011) Transport of solar wind fluctuations: a two-component model. J Geophys Res 116(A8)Google Scholar
  4. 4.
    Verdini A, Grappin R (2016) Beyond the maltese cross: geometry of turbulence between 0.2 and 1 au. Astrophys J 831(2):1–8Google Scholar

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© Springer Nature Switzerland AG 2019

Authors and Affiliations

  1. 1.Department of Surface and Plasma ScienceCharles UniversityPragueCzech Republic

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