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Formation and Topology of Foreshock Bubbles
Author(s) -
Omidi N.,
Lee S. H.,
Sibeck D. G.,
Turner D. L.,
Liu T. Z.,
Angelopoulos V.
Publication year - 2020
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
eISSN - 2169-9402
pISSN - 2169-9380
DOI - 10.1029/2020ja028058
Subject(s) - foreshock , physics , solar wind , bow shock (aerodynamics) , interplanetary magnetic field , classification of discontinuities , shock (circulatory) , magnetic field , computational physics , geophysics , mechanics , shock wave , geology , seismology , aftershock , medicine , mathematical analysis , mathematics , quantum mechanics
We use global and local hybrid (kinetic ions and fluid electrons) simulations to investigate the conditions under which foreshock bubbles (FBs) form and how their topology changes with solar wind conditions. FBs form as a result of the interaction between solar wind discontinuities and backstreaming ion beams in the foreshock. They consist of an outer shock and its associated sheath plasma and a low density high temperature core with low magnetic field strength. The structure of FBs is determined by the angle between the interplanetary magnetic field and the normal to the solar wind discontinuity. We show that interaction of rotational discontinuities with the foreshock during small angles between the interplanetary magnetic field and discontinuity normal results in the formation of a nearly spherical bubble with a radius that scales with the width of the foreshock. As this angle increases, FBs become more elongated and eventually become nearly planar structures with dimensions that scale with the length of the foreshock. Despite this transformation, the signatures of FBs in spacecraft time series data remain the same in agreement with the observations. Global simulation results show that FBs form when the solar wind flow speed corresponds to high or intermediate Alfvén Mach numbers (approximately >7 M A ). In general, this is tied to the relative speed between the solar wind and ion beams and drop in density of the backstreaming ions.