SH039-08
Combined observations of the heliospheric current sheet with Solar Orbiter and Parker Solar Probe
Monday, 14 December 2020: 11:58
Virtual
Benoit Lavraud1, Naïs Fargette1, Philippe Louarn2, Andrei Fedorov2, Alexis P Rouillard3, Vincent N Genot4, Roberto Bruno5, Lubomir Prech6, Stefano A Livi7, Christopher John Owen8, Virginia Angelini9, Stuart Bale10, Jonathan P Eastwood11, Vincent Evans9, Timothy Simon Horbury12, Jia Huang13, Justin Christophe Kasper13, Rungployphan Kieokaew14, Ronan Laker12, Helen O'Brien12, Emmanuel Penou15, Tai D. Phan16, Rui Pinto3, Illya Plotnikov1, Victor Réville1, Sergio Toledo-Redondo17 and Solar Orbiter and Parker Solar Probe teams, (1)IRAP, Toulouse, France, (2)IRAP, CNRS, Toulouse, France, (3)IRAP/CNRS, Toulouse, France, (4)IRAP / CNRS / UPS, PEPS, Toulouse, France, (5)INAF-IFSI, Rome, Italy, (6)Charles University Prague, Prague 8, Czech Republic, (7)SwRI, San Antonio, TX, United States, (8)University College London, Mullard Space Science Laboratory, Dorking, United Kingdom, (9)Imperial College London, Department of Physics, London, United Kingdom, (10)University of California, Berkeley, Berkeley, CA, United States, (11)Imperial College London, Physics, London, SW7, United Kingdom, (12)Imperial College London, Department of Physics, London, SW7, United Kingdom, (13)University of Michigan, Climate and Space Sciences and Engineering, Ann Arbor, MI, United States, (14)Mahidol University, Bangkok, Thailand, (15)Universite Paul Sabatier, TOULOUSE, France, (16)SSL, Berkeley, Berkeley, United States, (17)University of Murcia, Murcia, Spain
Abstract:
We will present recent observations from ESA’s Solar Orbiter and NASA’s Parker Solar Probe of heliospheric current sheet crossings in the inner heliosphere. With the help of modelling tools, we will compare in situ observations of the structure of the heliospheric current sheet and plasma sheet at the two spacecraft. In the light of recent works that suggest the predominant role of reconnection at the tip of the helmet streamer in structuring the HCS and HPS, we will determine how reconnection signatures evolve during propagation in the inner heliosphere.
