Abstract
The solar wind carves a cavity in the flow of interstellar H atoms through the solar system by charge-exchange ionization. The resulting Ly-α sky pattern depends on the latitude distribution of the solar wind flux and velocity. We review how the solar wind characteristics (mass flux latitude distribution) can be retrieved from Ly-α observations, yielding a new remote sensing method of solar wind studies, through UV optical measurements.
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Bertaux, J.L., Lallement, R. & Quemeelais, E. UV studies and the solar wind. Space Sci Rev 78, 317–328 (1996). https://doi.org/10.1007/BF00170818
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DOI: https://doi.org/10.1007/BF00170818