Identifying The Ends Of High-Speed Streams Near 1 AU With In Situ Data From STEREO/PLASTIC

Details Identifying The Ends Of High-Speed Streams Near 1 AU With In Situ Data From STEREO/PLASTIC Identifying The Ends Of High-Speed Streams Near 1 AU With In Situ Data From STEREO/PLASTIC

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216..351s&link_type=abstract

TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 351-354 (2010).

Computer Science

Solar Wind, Entropy, Solar Corona, Particle Emission, Solar Wind, Interface And Surface Thermodynamics, Corona

Scientific paper

The transition from fast to slow solar wind has not been studied to the same extent as the transition from slow to fast streams: the stream interface. The fast-to-slow transition has been reported as a smaller-scale mirror image of a stream interface. It is characterized by changes in speed, density, temperature, and composition (Geiss et al. 1995; Zurbuchen et al. 1999; Burlaga, Mish, and Whang 1990; Siscoe and Intriligator 1993; Burton et al. 1999). In this study we use solar wind ion data from STEREO/PLASTIC to further investigate the fast-to-slow wind interface, with particular emphasis on possible correlations between changes in the proton specific entropy argument and the solar wind's flow direction. The data were obtained during solar minimum near 1 AU and in the ecliptic plane. We find the fast-to-slow transition derived from the change in flow angle is neither as extended as the change in compositional signatures near 1 AU, nor as abrupt as that based on entropy at 4.5 to 5 AU.

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