Energy Transfer by Nonlinear Alfv’en Waves in the Solar Chromosphere, and Its Effect on Spicule Dynamics, Coronal Heating, and Solar Wind Acceleration. (arXiv:2008.00643v1 [astro-ph.SR])

Energy Transfer by Nonlinear Alfv’en Waves in the Solar Chromosphere, and Its Effect on Spicule Dynamics, Coronal Heating, and Solar Wind Acceleration. (arXiv:2008.00643v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sakaue_T/0/1/0/all/0/1">Takahito Sakaue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shibata_K/0/1/0/all/0/1">Kazunari Shibata</a>

Alfv’en waves are responsible for the transfer of magnetic energy in the
magnetized plasma. They are involved in heating solar atmosphere and driving
solar wind through various nonlinear processes. Since the magnetic field
configurations directly affect the nonlinearity of Alfv’en waves, it is
important to investigate how they relate to the solar atmosphere and wind
structure through the nonlinear propagation of Alfv’en waves. In this study,
we carried out the one-dimensional magnetohydrodynamic simulations to realize
the above relation. The results show that when the nonlinearity of Alfv’en
waves in the chromosphere exceeds a critical value, the dynamics of the solar
chromosphere (e.g., spicule) and the mass loss rate of solar wind tend to be
independent of the energy input from the photosphere. In a situation where the
Alfv’en waves are highly nonlinear, the strong shear torsional flow generated
in the chromosphere “fractures” the magnetic flux tube. This corresponds to
the formation of chromospheric intermediate shocks, which limit the
transmission of the Poynting flux into the corona by Alfv’en waves and also
inhibits the propagation of chromospheric slow shock.

Alfv’en waves are responsible for the transfer of magnetic energy in the
magnetized plasma. They are involved in heating solar atmosphere and driving
solar wind through various nonlinear processes. Since the magnetic field
configurations directly affect the nonlinearity of Alfv’en waves, it is
important to investigate how they relate to the solar atmosphere and wind
structure through the nonlinear propagation of Alfv’en waves. In this study,
we carried out the one-dimensional magnetohydrodynamic simulations to realize
the above relation. The results show that when the nonlinearity of Alfv’en
waves in the chromosphere exceeds a critical value, the dynamics of the solar
chromosphere (e.g., spicule) and the mass loss rate of solar wind tend to be
independent of the energy input from the photosphere. In a situation where the
Alfv’en waves are highly nonlinear, the strong shear torsional flow generated
in the chromosphere “fractures” the magnetic flux tube. This corresponds to
the formation of chromospheric intermediate shocks, which limit the
transmission of the Poynting flux into the corona by Alfv’en waves and also
inhibits the propagation of chromospheric slow shock.

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