Exploring with Multiple Spacecraft the Scene of the Traveling Strong Shock and its Driver

Details Exploring with Multiple Spacecraft the Scene of the Traveling Strong Shock and its Driver Exploring with Multiple Spacecraft the Scene of the Traveling Strong Shock and its Driver

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh31d..07b&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH31D-07

Physics

[2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2114] Interplanetary Physics / Energetic Particles, [2139] Interplanetary Physics / Interplanetary Shocks, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

We explore the global morphology of the transient shock generated by a fast solar ejection using multispacecraft observations, at wide heliographic longitudes. We consider the gradual solar energetic particle [SEP] events starting on 24 September 1977, 1 January and 23 September 1978, 26 March and 24 April 1979. To do this we use the solar wind parameters at each spacecraft location at the time of passage of the shock. In most cases data coverage at each shock passage enable us to estimate the shock normal and its velocity relative to the upstream solar wind. We remote sense the source of type II radio bursts, when available. Here, for each case, at the nearest in-situ location to the shocks nose, we present the findings; (1) the presence of unusual fast and massive driver, within two hours or less of the shock passage and the preliminary analysis of their unique plasma properties available, (2) with regard to the driven shock, with the help of modeling the inference of its morphological nature; (3) Further, the finding that each one of these five shocks has a surface portion moving at least more than 300 km/s faster than the upstream solar wind, enabling strong shock conditions, as we know from the Earth's bow shock, which are identified over distances from the Sun of 0.4 to 1.0 AU. Finally we show that the shock with the most extended and fastest surface portion (> 1600 km/s) is the one which produced the largest energetic proton flux in each energy channel (< 60 MeV), at each location within an extension of close to 180° in longitude. The shock with the smallest increase in energetic particle intensities, which was limited to an extension in longitude of less than 120°, had its fastest surface portion moving at possibly less than 900 km/s.

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