000007055 001__ 7055
000007055 005__ 20240919181300.0
000007055 037__ $$aPOSTER-2024-0077
000007055 100__ $$aMagdalenic, Jasmina
000007055 245__ $$aSolar wind modelling with EUHFORIA and the PSP observations
000007055 260__ $$c2024
000007055 269__ $$c2024-09-11
000007055 520__ $$aThe recently available observations of the solar wind by Parker Solar Probe (PSP) at close to the Sun distances show large variations. Majority of attempts to model solar wind with EUHFORIA (European heliospheric forecasting information asset, Pomoell & Poedts, 2018), along the PSP trajectory, provided not very accurate modelling results. In attempt to understand the source of this inaccuracy, we studied the solar wind observed during the first ten perihelion of PSP. Number of intervals of enhanced solar wind velocity appearing simultaneously with the decrease of the solar wind density was found, indicating that this solar wind is originating from the coronal holes. Employing the magnetic connectivity tool (developed by ESA’s MADAWG group) we confirmed the sources of that enhanced solar wind to be small coronal holes. In this study we present the characteristics of the solar wind flows originating from such a small coronal holes and compare them with characteristics of the fast solar wind originating from the large coronal holes, at close to the Sun distances. We discuss on the possible reasons for the lack of the fast solar wind in the PSP observations. In addition, we compare the characteristics of solar wind observed at close to the Sun distances and at 1 au.
000007055 536__ $$a2BRAIN_SWIM/$$c2BRAIN_SWIM/$$f2BRAIN_SWIM
000007055 594__ $$aNO
000007055 6531_ $$aSolar wind modeling, EUHFORIA, PSP
000007055 700__ $$aSenthamizh Pavai, Valliappan
000007055 773__ $$tESPM, Turin, Italy
000007055 8560_ $$fpavai.valliappan@ksb-orb.be
000007055 85642 $$ahttps://indico.ict.inaf.it/event/2553/abstracts/4138/
000007055 980__ $$aCPOSTER