Remote sensing of mercury sodium exospheric patterns in relation to particle precipitation and interplanetary magnetic field.

9 show that the peak distance is slightly different if we compute it for | B | < 24 nT, being maximum occurrence at 1.2 Mercury radii ( R M ), and for |IMF| > 24 nT, being peak distances maximum occurrence at 1.3 R M , identifying an increasing trend in the distance of the peaks with increasing | B | .

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The existence of a clear trend (correlation = 0.7706; critical limit= 0.7070) is confirmed if we look at right panel (c) that includes only cases where | B | is < 22 nT, confirming the expectation that the two peaks are better defined when Bz/ | B | is negative.

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