- Conference date: 17–22 June 2012
- Location: Big Island, Hawaii
Although the mechanisms responsible for heating the Sun's corona and accelerating the solar wind are being actively investigated, it is largely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process. 3D MHD models of the corona and of the solar wind usually employ some phenomenological artifice to accelerate the wind and heat the corona. Within the framework of a 3D full MHD numerical code, we apply the results of Rappazzo et al.  on turbulent cascade to heat the closed-field region, and those of Verdini and Velli , Verdini et al.  on Alfvén turbulence dissipation to accelerate the solar wind. We also compare the properties of the solar wind at 1 A.U. using a formulation based on Verdini and Velli , Verdini et al.  and one based on Chandran et al. .
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