Group Meeting

Orbit in Heliographic Coordinates

ENLIL simulation

Normalized solar wind density at the ecliptic and the IMF lines

Radial solar wind velocity at the ecliptic on the global and detail regions together with the temporal profile at spacecraft

Tab 1
Tab 2

Tab 1
Tab 2

Tab 1
Tab 2

Perrone et al. (2019)

The radial dependence of the proton number density, $n_{p}$ and magnetic ﬁeld magnitude, $B$ , is given by

n_{p} = (2.4 \pm 0.1) (R / R_{0})^{- (1.96 \pm 0.07)} c m^{- 3}

B = (5.7 \pm 0.2) (R / R_{0})^{- (1.59 \pm 0.06)} n T

The faster decrease of the magnetic than kinetic pressure is reﬂected in the radial proton plasma beta variation

β_{p} = P_{k} / P_{B} = (0.55 \pm 0.04) (R / R_{0})^{(0.4 \pm 0.1)} .

References

Perrone, Denise, D Stansby, T S Horbury, and L Matteini. 2019. “Radial Evolution of the Solar Wind in Pure High-Speed Streams: HELIOS Revised Observations.” Monthly Notices of the Royal Astronomical Society 483 (3): 3730–37. https://doi.org/10.1093/mnras/sty3348.