Kinetic Alfvén wave and ion velocity distribution functions in the solar wind

Details Kinetic Alfvén wave and ion velocity distribution functions in the solar wind Kinetic Alfvén wave and ion velocity distribution functions in the solar wind

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41b1788l&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH41B-1788

Physics

Plasma Physics

[2164] Interplanetary Physics / Solar Wind Plasma, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7829] Space Plasma Physics / Kinetic Waves And Instabilities, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

Using 1D test particle simulations, the effect of a kinetic Alfvén wave on the velocity distribution function of protons in the collisionless solar wind is investigated. We first use linear Vlasov theory to obtain the property of a kinetic Alfvén wave numerically (the wave propagates in the direction almost perpendicular to the background magnetic field). We then numerically simulate how the wave will shape the proton velocity distribution function. It is found that Landau resonance may be able to generate two components in the initially Maxwellian proton velocity distribution function: a tenuous beam component along the direction of the background magnetic field and a core component. The streaming speed of the beam relative to the core proton component is about 1.2 -- 1.3 Alfvén speed. However, no perpendicular ion heating is observed from the simulation. Reference: Li, X., Lu, Q.M., Chen, Y., Li, B., Xia, L.D., ApJ, 719, L190, 2010.

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