Ion Heating across the Magnetic Field in the Solar Corona by Kinetic Alfvén Waves

Details Ion Heating across the Magnetic Field in the Solar Corona by Kinetic Alfvén Waves Ion Heating across the Magnetic Field in the Solar Corona by Kinetic Alfvén Waves

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547..381v&link_type=abstract

Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a

Computer Science

Solar Corona, Alfvén Waves, Stochastic Heating

Scientific paper

The perpendicular heating of the ions observed by SOHO in the solar corona at 2-4 solar radii has been mainly attributed to the ion-cyclotron damping of high-frequency Alfvén waves. We investigate an alternative mechanism of heating by low-frequency Alfvén waves that have short wavelengths across the magnetic field - kinetic Alfvén waves (KAWs). The energy reservoir for these kinetic waves is provided by low-frequency large-scale MHD waves that are launched in the corona by the photospheric motions or excited at the coronal base by magnetic restructuring. The short perpendicular wavelengths, developed by phase mixing, convert MHD Alfvén waves into KAWs. KAWs can be also excited in situ by various linear and nonlinear mechanisms. We show that above a threshold value of the wave amplitude, KAWs can stochastically accelerate ions across the background magnetic field. In particular, KAWs with transversal wavelengths of the order of the ion inertial length and with a wave/background magnetic field ratio of the order 0.1, can contribute to the stochastic heating of oxygen ions O5+ . We discuss advantages of this mechanism over the ion-cyclotron heating scheme for the intense transverse heating of ions observed by SOHO at 2-4 solar radii.

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