Numerical simulations of the solar wind transients in terms of the spacecraft position
Abstract
Several numerical models have been developed for a better understanding of the dynamical evolution, propagation and possible interaction among solar wind transients, such as Coronal Mass Ejections (CMEs) and Co-rotating Interaction Regions (CIRs). In general, the evolution of these transients depend on both the initial conditions of each of them and the properties of the ambient solar wind. The number of free parameters used as inputs in the models causes uncertainties in forecasting, which increase when interactions take place. Most of the numerical models have good results in predicting the arrival time and speed at 1 AU, but their performance is relatively poor in terms of the time profile morphology of the in-situ parameters. In this work, we performed several 2D numerical simulations -using a hydrydynamic code- to predict the time profile morphology of the in-situ parameters of different type of transients: a single CME, a single CIR, and complex structures due to the CME-CME and CIR-CME interactions. We compare the theoretical profiles with observations at 1 AU of these sort of sources. In particular, we focus on the morphology changes as function of the angular distance between the radial direction of the CME and the observer position. This analysis can be useful to understand the geo-effectiveness of these transient events.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2017
- Bibcode:
- 2017AGUFMSH53A2544G
- Keywords:
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- 2101 Coronal mass ejections;
- INTERPLANETARY PHYSICS;
- 2102 Corotating streams;
- INTERPLANETARY PHYSICS;
- 2111 Ejecta;
- driver gases;
- and magnetic clouds;
- INTERPLANETARY PHYSICS;
- 2162 Solar cycle variations;
- INTERPLANETARY PHYSICS