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The Magnetic cloud boundary layer (BL) is a dynamic region formed by theinteraction of the magnetic cloud (MC) and the ambient solar wind. In thepresent study, we comparatively investigate the proton and electron mean fluxvariations in the BL, in the interplanetary reconnection exhaust (RE) andacross the MC-driven shock by using the Wind 3DP and MFI data from 1995 to2006. In general, the proton flux has higher increments at lower energy bandscompared with the ambient solar wind. Inside the BL, the core electron fluxincreases quasi-isotropically and the increments decrease monotonously withenergy from ~30% (at 18 eV) to ~10% (at 70 eV); the suprathermal electron fluxusually increases in either parallel or antiparallel direction; the correlationcoefficient of electron flux variations in parallel and antiparallel directionschanges sharply from ~0.8 below 70 eV to ~0 above 70 eV. Similar results arealso found for RE. However, different phenomena are found across the shockwhere the electron flux variations first increase and then decrease with a peakincrement (>200%) near 100 eV. The correlation coefficient of electron fluxvariations in parallel and antiparallel directions is always around 0.8. Thesimilar behavior of flux variations in BL and RE suggests that reconnection maycommonly occur in BL. Our work also implies that the strong energy dependenceand direction selectivity of electron flux variations, which are previouslythought to have no enough relevance to magnetic reconnection, could beconsidered as an important signature of solar wind reconnection in thestatistical point of view.

astrophysical journal/the astrophysical journal

Variations of solar electron and proton flux in magnetic cloud boundary  layers and comparisons with those across the shocks and in the reconnection  exhausts