Magnetosheath jet evolution as a function of lifetime: global hybrid-Vlasov simulations compared to MMS observations

• Published in: Annales geophysicae (1988) 2021-03, Vol.39 (2), p.289-308
• Main Authors: Palmroth, Minna, Raptis, Savvas, Suni, Jonas, Karlsson, Tomas, Turc, Lucile, Johlander, Andreas, Ganse, Urs, Pfau-Kempf, Yann, Blanco-Cano, Xochitl, Akhavan-Tafti, Mojtaba, Battarbee, Markus, Dubart, Maxime, Grandin, Maxime, Tarvus, Vertti, Osmane, Adnane
• Format: Article
• Language: English
• Subjects: Comparative analysis; Datasets; Dimensions; Dynamic pressure; Flow velocity; Investigations; Jets; Mach number; Magnetic field; Magnetic fields; Magnetic flux; Magnetopause; Magnetosheath; Magnetosphere; Magnetospheres; MMS (Multimedia messaging service); Parameter estimation; Parameters; Physics; Plasma; Pressure; Shock; Simulation; Solar wind; Spacecraft; Statistical methods; Velocity
• ISSN: 1432-0576; 0992-7689; 1432-0576
• DOI: 10.5194/angeo-39-289-2021

Magnetosheath jets are regions of high dynamic pressure, which can traverse from the bow shock towards the magnetopause. Recent modelling efforts, limited to a single jet and a single set of upstream conditions, have provided the first estimations about how the jet parameters behave as a function of position within the magnetosheath. Here we expand the earlier results by doing the first statistical investigation of the jet dimensions and parameters as a function of their lifetime within the magnetosheath. To verify the simulation behaviour, we first identify jets from Magnetosphere Multiscale (MMS) spacecraft data (6142 in total) and confirm the Vlasiator jet general behaviour using statistics of 924 simulated individual jets. We find that the jets in the simulation are in quantitative agreement with the observations, confirming earlier findings related to jets using Vlasiator. The jet density, dynamic pressure, and magnetic field intensity show a sharp jump at the bow shock, which decreases towards the magnetopause. The jets appear compressive and cooler than the magnetosheath at the bow shock, while during their propagation towards the magnetopause they thermalise. Further, the shape of the jets flatten as they progress through the magnetosheath. They are able to maintain their flow velocity and direction within the magnetosheath flow, and they end up preferentially to the side of the magnetosheath behind the quasi-parallel shock. Finally, we find that Vlasiator jets during low solar wind Alfvén Mach number MA are shorter in duration, smaller in their extent, and weaker in terms of dynamic pressure and magnetic field intensity as compared to the jets during high MA.