Reconstruction of the Parker spiral with the Reverse in situ data and MHD APproach - RIMAP
| Autor: | R. Biondo, Alessandro Bemporad, Andrea Mignone, Fabio Reale |
|---|---|
| Přispěvatelé: | Biondo R., Bemporad A., Mignone A., Reale F. |
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Atmospheric Science
010504 meteorology & atmospheric sciences Space weather Solar wind Interplanetary medium lcsh:QC851-999 01 natural sciences Heliosphere 0103 physical sciences Coronal mass ejection Astrophysics::Solar and Stellar Astrophysics 010303 astronomy & astrophysics 0105 earth and related environmental sciences Physics Modeling Coronal mass ejections Computational physics Space and Planetary Science Physics::Space Physics lcsh:Meteorology. Climatology Heliospheric current sheet Astrophysics::Earth and Planetary Astrophysics Magnetohydrodynamics Interplanetary spaceflight |
| Zdroj: | Journal of Space Weather and Space Climate, Vol 11, p 7 (2021) |
| Popis: | The reconstruction of plasma parameters in the interplanetary medium is very important to understand the interplanetary propagation of solar eruptions and for Space Weather application purposes. Because only a few spacecraft are measuring in situ these parameters, reconstructions are currently performed by running complex numerical Magneto-hydrodynamic (MHD) simulations starting from remote sensing observations of the Sun. Current models apply full 3D MHD simulations of the corona or extrapolations of photospheric magnetic fields combined with semi-empirical relationships to derive the plasma parameters on a sphere centered on the Sun (inner boundary). The plasma is then propagated in the interplanetary medium up to the Earth’s orbit and beyond. Nevertheless, this approach requires significant theoretical and computational efforts, and the results are only in partial agreement with the in situ observations. In this paper we describe a new approach to this problem called RIMAP – Reverse In situ data and MHD APproach. The plasma parameters in the inner boundary at 0.1 AU are derived directly from the in situ measurements acquired at 1 AU, by applying a back reconstruction technique to remap them into the inner heliosphere. This remapping is done by using the Weber and Davies solar wind theoretical model to reconstruct the wind flowlines. The plasma is then re-propagated outward from 0.1 AU by running a MHD numerical simulation based on the PLUTO code. The interplanetary spiral reconstructions obtained with RIMAP are not only in a much better agreement with the in situ observations, but are also including many more small-scale longitudinal features in the plasma parameters that are not reproduced with the approaches developed so far. |
| Databáze: | OpenAIRE |
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