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Deconvolution of the Shock Front Speed Profile into Blast Waves in the Solar Wind

机译：将冲击前速度剖面反演为太阳风中的爆炸波

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We find that the in-situ space observations and the computer MHD simulation support the concept that the propagation of the front of the solar-flare initiated shock disturbance through interplanetary space can be deconvolved into two separable components. These are the shock front resulting from the impulsive release of energy from a solar flare and the pre-existing solar wind. These two speeds vectorially combine to yield the disturbance speed toward the observation location. By separating the average sun-earth disturbance speed into two components, we have an average blast wave speed and the solar wind speed. This decoupling of the shock front speed and the solar wind speed is similar in concept to calculating the shock speed from in-situ spacecraft plasma and field measurements by applying the Rankine-Hugoniot conditions. From our empirical deconvolution of the solar-flare-initiated shock into separable components we find that a general characteristic of the shock front speed profile in the solar wind frame is a slope of -0.5, the same as expected for a blast wave.

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