This paper describes coronal inflows observed with the Large Angle Spectrometric Coronagraph (LASCO). The inflows are not seen above 5.5 R☉, which appears to be a "point of no return" for the Sun's plasmas and fields. Below this height, most inflows seem to indicate magnetic flux that is returning to the Sun after its reconnection at sector boundaries. Some inflows have characteristics (like fast, oppositely directed ejections of material) that are easily interpreted in terms of conventional models of field line reconnection. However, the overwhelming majority of coronal inflows have a more complex behavior that typically includes the following characteristics:
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Sheeley et al. (2002) studied this question.
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