Computer Science
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..554f&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 554
Computer Science
9
Solar Wind Plasma, Sources Of Solar Wind, Interplanetary Magnetic Fields
Scientific paper
Fifteen years ago, Burlaga defined magnetic clouds as interplanetary structures with enhanced magnetic field characterized by a smooth rotation of the magnetic field vector and a low proton temperature Tp. Their expansion in the solar wind leads to a depletion of plasma and a cooling of the ion component. Recently, Osherovich and colleagues showed that the electron component in magnetic clouds behaves differently: When the cloud expands, the electron temperature Te anticorrelates with the density and therefore Te increases in the cloud. Since Landau damping is not effective for Te/Tp>>1, they predicted an increase of ion-acoustic wave activity in magnetic clouds. Our paper presents evidence in support of this prediction. For the magnetic cloud observed by Ulysses on June 10-12, 1993 at 4.64 AU at S 32.5 deg, we present observations for both the electron and the proton components and the related plasma waves activity. Our results confirm the anticorrelation between Te and electron density: the data also exhibit high ratios of Te/Tp in the cloud (Te/Tp~10-20). Calculated frequencies of Doppler-shifted ion-acoustic waves compare well with the frequency range of the observed wave activity in the cloud. We find that the electron component in the cloud obeys a polytropic law with polytropic index γe<1(γe~0.35-0.37). The dynamics of this magnetic cloud are determined to a large degree by the dominating electron pressure with the contribution from halo electrons comparable to that from core electrons.
Balogh André
Fainberg Joe
Macdowall Robert J.
Osherovich Vladimir A.
Stone Robert G.
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