Signatures of turbulent heating in heavy-ion velocity distribution functions

Details Signatures of turbulent heating in heavy-ion velocity distribution functions Signatures of turbulent heating in heavy-ion velocity distribution functions

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh41c..04b&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH41C-04

Physics

2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma

Scientific paper

The kinetic properties of the solar wind are a result of complex interactions in the solar corona and interplanetary space. Sofar, observations of velocity distribution functions (VDFs) of solar wind heavy ions have been solely 1D. They are known to exhibit non-thermal features , but because they are 1D projections of the 3D velocity phase space it is difficult to interpret them properly. Based on 3D observations of H+ and He2+ from Helios, we have set up a model for heavy-ion VDFs. In it, the magnetic field vector plays a crucial role by defining the symmetry axis of the VDFs. A thermal anisotropy T⊥/T∥≠1 and a beam drifting along the magnetic field vector at a relative speed of approximately the Alfvèn speed are included. The modeled VDFs are analyzed using a virtual detector and then compared with ACE/SWICS data. Our observations give striking evidence for turbulent heating and the existence of heavy-ion beams. The projection of these beams can explain observed differential streaming. We present in-situ measurements at 1 AU and implications for wave-paricle interactions between the Sun and Earth.

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