Observation of saturnian stream particles in the interplanetary space

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• 作者：Hsiang-Wen Hsu ; Sascha Kempf ; Caitriona M. Jackman
• 关键词：Saturn ; Solar wind ; Magnetic fields
• 刊名：Icarus
• 出版年：2010
• 出版时间：April 2010
• 年：2010
• 卷：206
• 期：2
• 页码：653-661
• 全文大小：1373 K

文摘

In January 2004 the dust instrument on the Cassini spacecraft detected the first high-velocity grain expelled from Saturn – a so-called stream particle. Prior to Cassini’s arrival at Saturn in July 2004 the instrument registered 801 faint impacts, whose impact signals showed the characteristic features of a high-velocity impact by a tiny grain. The impact rates as well as the directionality of the stream particles clearly correlate with the sector structure of the interplanetary magnetic field (IMF). The Cosmic Dust Analyser (CDA) registered stream particles dominantly during periods when the IMF direction was tangential to the solar wind flow and in the prograde direction. This finding provides clear evidence for a continuous outflow of tiny dust grains with similar properties from the saturnian system. Within the compressed part of co-rotating interaction regions (CIRs) of the IMF, characterized by enhanced magnetic field strength and compressed solar wind plasma, CDA observed impact bursts of faster stream particles. We find that the bursts result from the stream particles being sped up inside the compressed CIR regions. Our analysis of the stream-particle dynamics inside rarefaction regions of the IMF implies that saturnian stream particles have sizes between 2 and 9 nm and exit the saturnian systems closely aligned with the planet’s ring plane with speeds in excess of 70 km s⁻¹.