Proton beam velocity distributions in an interplanetary coronal mass ejection

Details Proton beam velocity distributions in an interplanetary coronal mass ejection Proton beam velocity distributions in an interplanetary coronal mass ejection

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009angeo..27..869m&link_type=abstract

Annales Geophysicae, Volume 27, Issue 2, 2009, pp.869-875

Physics

4

Scientific paper

The plasma and magnetic-field instruments on the Helios 2 spacecraft, which was on 3 April 1979 located at 0.68 AU, detected an interplanetary coronal mass ejection (ICME) that revealed itself by the typical signature of magnetic field rotation. The solar wind flow speed ranged between 400 and 500 km/s. We present here some detailed proton velocity distributions measured within the ICME. These cold distributions are characterized by an isotropic core part with a low temperature, T≤105 K, but sometimes reveal a broad and extended hot proton tail or beam propagating along the local magnetic field direction. These beams lasted only for about an hour and were unusual as compared with the normal ICME protons distribution which were comparatively isotropic. Furthermore, we looked into the velocity and field fluctuations in this ICME and found signatures of Alfvén waves, which might be related to the occurrence of the hot proton beams. However, it cannot be excluded that the beam originated from the Sun.

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