Dynamics of Slow Solar Wind Emerging from an Equatorial Coronal Hole

Le résumé fourni par la source

Abstract We present a three-dimensional reduced magnetohydrodynamics model to depict turbulence induced by Alfvén waves within the slow solar wind originating from an open magnetic field positioned in a coronal hole near the solar equator. The nonlinear interactions between outward- and inward-propagating waves result in turbulence. As part of this investigation, we examine the conditions prevailing in an equatorial coronal hole using the interplanetary scintillation (IPS) observations. From IPS observations, we measure the magnetic field and velocity, both input parameters of our Alfvén wave turbulence model. We show the conditions of equatorial corona, a contributor to the slow solar wind, can generate Alfvén wave turbulence that accelerates and energizes the slow wind.

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