Fig. 9
From: A new view on the solar wind interaction with the Moon
Profiles of backscattered protons and the solar wind protons for the period 12 June to 2 July 2009. a The proton flux profile, where the crosses represent the backscattered protons observed by SWIM/CH-1 and the thick line is representative of solar wind protons from Wind/Solar Wind Experiment (SWE). The fractions −1 and 0.1 % of solar wind proton flux are indicated using thin lines. The expected contribution from the instrument background is shown as ‘Background level’. b The density and speed of the solar wind protons obtained from Wind/SWE. c The interplanetary magnetic field from Wind/SWE. The intervals having lowest and highest solar wind speeds are indicated by shaded fields [from Lue et al. (2014)]