Computer Science
Scientific paper
Mar 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216..253b&link_type=abstract
TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 253-256 (2010).
Computer Science
Interplanetary Magnetic Fields, Solar Corona, Solar Wind, Solar Magnetism, Solar Wind Plasma, Sources Of Solar Wind, Corona, Particle Emission, Solar Wind, Magnetic And Electric Fields, Polarization Of Starlight
Scientific paper
The kinetic properties of the solar wind are a result of complex interactions in the solar corona and interplanetary space. So far, 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 protons and alpha particles 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 Alfvén speed are included. The modeled VDFs are analysed using a virtual detector and then compared with data from the Solar Wind Ion Composition Spectrometer (SWICS) on the Advanced Composition Explorer (ACE). Our observations give evidence for the existence of heavy-ion beams. The projection of these beams can explain observed differential streaming. We present in-situ measurements and derived kinetic properties of O6+ at 1 AU.
Berger Laurent
Gloeckler George
Wimmer-Schweingruber Robert F.
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