SH039-09
A joint study of Solar Orbiter first data and PSP E5 through 3D MHD modeling
Monday, 14 December 2020: 12:02
Virtual
Victor Réville1, Antoine Strugarek2, Sacha Brun3, Alexis P Rouillard4, Marco C M Velli5, Nicolas Poirier1, Susanna Parenti6, Soumitra Hazra7, Barbara Perri8, Rui Pinto4, Benoit Lavraud4, Philippe Louarn9, Andrei Fedorov9, Christopher John Owen10, Roberto Bruno11, Roberto Livi12, Timothy Simon Horbury13, Helen O'Brien13, Vincent Evans14, Virginia Angelini14, Stuart D Bale15, Justin Christophe Kasper16 and Solar Orbiter and Parker Solar Probe, (1)IRAP, Toulouse, France, (2)DRF/IRFU/DAp/LDE3 CEA Saclay, Saclay, France, (3)CEA Commissariat à l'Energie Atomique Saclay, Gif-Sur-Yvette Cedex, France, (4)IRAP/CNRS, Toulouse, France, (5)University of California Los Angeles, Los Angeles, CA, United States, (6)Institut d'Astrophysique de Paris, Paris, France, (7)Georgia State University, Department of Physics & Astronomy, Atlanta, GA, United States, (8)IAS Institut d'Astrophysique Spatiale, Orsay Cedex, France, (9)IRAP, CNRS, Toulouse, France, (10)University College London, Mullard Space Science Laboratory, Dorking, United Kingdom, (11)INAF-IFSI, Rome, Italy, (12)Space Sciences Laboratory, University of California Berkeley, Berkeley, CA, United States, (13)Imperial College London, Department of Physics, London, SW7, United Kingdom, (14)Imperial College London, Department of Physics, London, United Kingdom, (15)University of California Berkeley, Space Sciences Laboratory, Berkeley, CA, United States, (16)University of Michigan, Climate and Space Sciences and Engineering, Ann Arbor, MI, United States
Abstract:
The first remote sensing window of Solar Orbiter started mid-June 2020. After a successful commissioning, Solar Orbiter in situ instruments were then continuously monitoring. This window is coincidentally close to the fifth perihelion of Parker Solar Probe. This offers an opportunity for a joint study between the two probes’ data. We use a 3D MHD model of a turbulence driven solar wind, and compare the structure of the inner heliosphere obtained by the model and the available in situ and remote sensing data of the spacecraft. We discuss the key features of the model and tricky points that require care, such as the choice of the input magnetogram. In particular, we notice the strong influence of two active regions on the magnetic sectors and solar wind properties. These regions will be increasingly important features in future encounters and joint studies as we go towards solar maximum.
