We have successfully reproduced the spectral anisotropy characteristic of slow and fast winds and associate them to the initial spectral anisotropy, cross helicity and radial expansion. We have also proven that, independently of the spectral anisotropy, turbulent heating is able to slow down the adiabatic cooling of the solar wind, giving a temperature evolution proportional to 1/R. Our results are commented in the context of the upcoming Parker Solar Probe and Solar Orbiter missions.
- 1.Dasso Milano LJ, Matthaeus WH, Smith CW (2005) Anisotropy in fast and slow Solar Wind Fluctuations. Astrophys J 635(2):L181–L184. https://doi.org/10.1086/499559
- 2.Fox NJ, Velli M, Bale S, Decker R, Driesman A, Howard R, Kasper JC, Kinnison J, Kusterer M, Lario D, Lockwood MK, McComas DJ, Raouafi NE, Szabo A (2016) The solar probe plus mission: humanity’s first visit to our star. Space Sci Rev 1–42: https://doi.org/10.1007/s11214-015-0211-6
- 9.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