Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind

dc.contributor.author	Wójcik, D.
dc.contributor.author	Kuźma, B.
dc.contributor.author	Murawski, K.
dc.contributor.author	Srivastava, A.K.
dc.date.accessioned	2020-12-17T11:24:46Z
dc.date.available	2020-12-17T11:24:46Z
dc.date.issued	2019-10-20
dc.identifier.issn	0004637X
dc.identifier.uri	http://localhost:8080/xmlui/handle/123456789/1186
dc.description.abstract	With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities that are consistent, to the order of magnitude, with the observational findings for mass and energy losses in the upper chromosphere, transition region, and inner corona, and they may originate the fast solar wind. © 2019. The American Astronomical Society. All rights reserved..	en_US
dc.language.iso	en_US	en_US
dc.publisher	Institute of Physics Publishing	en_US
dc.relation.ispartofseries	Astrophysical Journal;Vol. 884 issue 2
dc.subject	magnetohydrodynamics (MHD) – methods	en_US
dc.subject	numerical – solar wind – Sun	en_US
dc.subject	activity – Sun	en_US
dc.subject	corona	en_US
dc.title	Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind	en_US
dc.type	Article	en_US