Two-fluid numerical simulations of the origin of the fast solar wind. (arXiv:1906.01897v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wojcik_D/0/1/0/all/0/1">D. W&#xf3;jcik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuzma_B/0/1/0/all/0/1">B. Ku&#x17a;ma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murawski_K/0/1/0/all/0/1">K. Murawski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Srivastava_A/0/1/0/all/0/1">A.K. Srivastava</a>

With the use of our JOANNA code, which solves radiative equations for ion +
electron and neutralfluids, we perform realistic 2.5D numerical simulations of
plasma outflows associated with the solargranulation. These outflows exhibit
physical quantities consistentto the order of magnitude with theobservational
findings for mass and energy losses in the upper chromosphere, transition
region andinner corona, and they may originate the fast solar wind.

With the use of our JOANNA code, which solves radiative equations for ion +
electron and neutralfluids, we perform realistic 2.5D numerical simulations of
plasma outflows associated with the solargranulation. These outflows exhibit
physical quantities consistentto the order of magnitude with theobservational
findings for mass and energy losses in the upper chromosphere, transition
region andinner corona, and they may originate the fast solar wind.

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