(Non)-radial propagation of the solar wind flow
- 1Charles University, Faculty of Mathematics and Physics, Department of Surface and Plasma Science, Prague 8, Czechia (nemecek@aurora.troja.mff.cuni.cz)
- 2Institute of Atmospheric Physics, Prague, Czech Republic
- 3Kavli Center for Astrophysics and Space Science, Massachusetts Institute of Technology, Cambridge, USA
The solar wind aberration due to non-radial velocity components and the Earth orbital motion is important for the overall magnetosphere geometry because the magnetospheric tail is aligned with the solar wind flow. This paper investigates an evolution of non-radial components of the solar wind flow along the path from the Sun to 6 AU. A comparison of observations at 1 AU and closer to or further from the Sun based on measurements of many spacecraft at different locations in the heliosphere (Wind, ACE, Spektr-R, THEMIS B and C, Helios 1 and 2, Mars-Express, Voyager 1 and 2) shows that (i) the average values of non-radial components vary with the distance from the Sun and (ii) they differ according to solar wind streams.
How to cite: Němeček, Z., Ďurovcová, T., Šafránková, J., Šimůnek, J., Richardson, J. D., and Urbář, J.: (Non)-radial propagation of the solar wind flow , EGU General Assembly 2020, Online, 4–8 May 2020, EGU2020-2736, https://doi.org/10.5194/egusphere-egu2020-2736, 2020.
