Magnetosheath Plasma Flow and Its Response to IMF and Geodipole Tilt as Obtained From the Data‐Based Modeling

• Published in: Journal of geophysical research. Space physics 2024-11, Vol.129 (11), p.n/a
• Main Authors: Tsyganenko, N. A., Semenov, V. S., Erkaev, N. V., Gubaidulin, N. T.
• Format: Article
• Language: English
• Subjects: Attitude (inclination); Axisymmetric flow; Charged particles; Coordinate systems; Coordinates; Corona; Earth magnetosphere; Earth orbits; Electromagnetic forces; Flow distribution; Flow geometry; Flow pattern; Geomagnetic field; Interplanetary magnetic field; Magnetic dipoles; Magnetic fields; Magnetopause; Magnetosheath; magnetosphere; Magnetospheric boundary; modeling; Particle transport; Plasma; reconnection; Satellite data; Solar corona; Solar magnetic field; Solar wind; Solar wind particles; Space missions; Spacecraft; Wind effects
• ISSN: 2169-9380; 2169-9402
• DOI: 10.1029/2024JA033233

Large‐scale patterns of the steady‐state magnetosheath plasma flow and their dependence on the interplanetary magnetic field (IMF) have been reconstructed for the first time on the basis of large multi‐year multi‐mission pool of spacecraft observations, concurrent interplanetary data, and an empirical high‐resolution model. The flow model architecture builds upon a recently developed magnetosheath magnetic field representation by flexible expansions of its toroidal and poloidal components in a coordinate system, naturally conformed with the magnetopause and bow shock shapes. The model includes two physics‐based flow symmetry modes: the first one treats the magnetosphere as an axisymmetric unmagnetized obstacle, whereas the second mode takes into account the geodipole tilt, an important factor in the reconnection effects. The spacecraft data pool includes 1‐min average data by Themis (2007–2024), Cluster (2001–2022), and MMS‐1 (2015–2024) missions, as well as OMNI interplanetary data. The model drivers include the solar wind particle flux, IMF components, and the geodipole tilt angle. The model calculations faithfully reproduce the average plasma flow geometry and substantial effects have been found of the IMF orientation and magnitude, a principal factor that defines electromagnetic forces inside the magnetosheath. A strong dependence of the magnetosheath flow patterns on the Earth's dipole tilt indicates an important contribution of reconnection effects at the magnetopause to the solar wind particle transport around the dayside magnetosphere. Plain Language Summary As a result of the solar wind interaction with the geomagnetic field, the Earth's magnetosphere becomes embedded within a huge “cocoon”, a vast region between the bow shock and the magnetopause, where the incoming plasma stream gets compressed, heated, and diverted sideways around the magnetospheric boundary. An important factor that significantly affects the magnetosheath flow is the interplanetary magnetic field (IMF), transported to the Earth's orbit from the solar corona. The IMF undergoes compression and deformation inside the magnetosheath; the resulting electromagnetic forces substantially affect the plasma flow. Furthermore, the magnetic fields of solar and terrestrial origin can reconnect at the magnetopause, which results in additional modifications of the plasma flow pattern. During the last decades, huge amounts of satellite data were obtained in the near‐Earth space; using them in