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Fig. 9 | Progress in Earth and Planetary Science

Fig. 9

From: A review of the SCOSTEP’s 5-year scientific program VarSITI—Variability of the Sun and Its Terrestrial Impact

Fig. 9

In situ observations of the 2017-09-10 events at Earth (left panels), Mars (f-h), and STA (ik). a, i The energy-dependent particle flux (counts/cm2/sr/MeV/sec) measured by GOES and STA. b Count rate of several ground-based neutron monitors with different cut-off rigidities (each neutron monitor data set is normalized to the average value of the selected time range and shifted apart in y-axis). c, h, and j The solar wind speed (black, left Y-axis (yl)), proton density (blue, right Y-axis (year)), and temperature (red, year) for Earth (OMNI), Mars (MEX), and STA, respectively. The ENLIL modeled results at three locations are also plotted as dashed lines. d Plots of the Alfvén Mach number (black, yl), plasma (blue, year), and flow pressure (red, year) estimated at Earth. e, k The vector magnetic fields at Earth/STA in Geocentric Solar Ecliptic (GSE) or spacecraft Radial-Tangential-Normal (RTN) coordinate and negative ENLIL modeled magnetic field strength (dashed line). f The normalized count rate for downward particles stopping in RAD and penetrating RAD with the former/later approximating protons with energies larger than 175/288 MeV arriving at Mars. g The dose rate recorded in RAD B (silicon) and E (plastic) detectors. Magenta-highlighted areas are the ICME and/or its associated shock passage at Earth and Mars. Cyan-highlighted areas are high-speed streams (of two different ones) passing Earth and STA during this period. Vertical solid lines in a, b, f, g, and i indicate the particle onset time at Earth/Mars/STA (taken from Guo et al. 2018)

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