Acceleration and heating of solar wind ions by turbulent wave spectrum

Details Acceleration and heating of solar wind ions by turbulent wave spectrum Acceleration and heating of solar wind ions by turbulent wave spectrum

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh43a1648o&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH43A-1648

Other

7509 Corona, 7524 Magnetic Fields, 7827 Kinetic And Mhd Theory, 7836 Mhd Waves And Instabilities (2149, 2752, 6050), 7863 Turbulence (4490)

Scientific paper

We model the heating and the acceleration of multi-ion plasma of the solar wind by turbulent spectrum of Alfvénic fluctuations in the resonant and nonresonant frequency range. The modeling effort is guided by the observed properties of the spectrum and the measured physical parameters of the solar wind plasma in the heliosphere in-situ, as well as close to the sun from remote sensing observations. We start with 2.5D multifluid model that includes ion-cyclotron terms to study the nonresonant wave heating and acceleration, and proceed with 2D hybrid model that extends into the resonant frequency range. In addition to protons the model includes helium ions, and other heavy ions, and the results of the turbulent Alfvénic wave spectrum is compared to observation. In the hybrid model the protons and heavy ions are treated kinetically, while the electrons are included as neutralizing background fluid. This model allows to extend the study to resonant frequency range, and explore the nonlinear saturation of the heating for resonant and nonresonant waves. The models are used to explore the effect of non-homogeneous background density across the magnetic field, and of ion beams on the heating by turbulent wave spectrum.

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