Remote and in situ observations strongly imply that the slow solar wind consists of plasma from the hot, closed-field corona that is released onto open magnetic field lines. The Separatrix Web theory for the slow wind proposesthat photospheric motions at the scale of supergranules are responsible for generating dynamics at coronal-holeboundaries, which result in the closed plasma release. We use three-dimensional magnetohydrodynamicsimulations to determine the effect of photospheric flows on the open and closed magnetic flux of a model coronawith a dipole magnetic field and an isothermal solar wind. A rotational surface motion is used to approximatephotospheric supergranular driving and is applied at the boundary between the coronal hole an...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
Remote and in situ observations strongly imply that the slow solar wind consists of plasma from the ...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
Remote and in situ observations strongly imply that the slow solar wind consists of plasma from the ...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
Context. The generation of the slow solar wind remains an open problem in heliophysics. One of the c...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...
The boundaries of solar coronal holes are difficult to uniquely define observationally but are sites...