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Estimating the effects of ionospheric plasma on solar wind/magnetosphere coupling via mass loading of dayside reconnection: Ion‐plasma‐sheet oxygen, plasmaspheric drainage plumes, and the plasma cloak
Author(s) -
Borovsky Joseph E.,
Denton Michael H.,
Denton Richard E.,
Jordanova Vania K.,
Krall Jonathan
Publication year - 2013
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
eISSN - 2169-9402
pISSN - 2169-9380
DOI - 10.1002/jgra.50527
Subject(s) - magnetopause , physics , solar wind , magnetosphere , ionosphere , geophysics , coronal mass ejection , magnetosheath , geosynchronous orbit , plasma , geomagnetic storm , atmospheric sciences , magnetic reconnection , computational physics , astronomy , satellite , quantum mechanics
Estimates are calculated for the storm time reduction of solar wind/magnetosphere coupling by the mass density ρ m of the magnetospheric plasma. Based on the application of the Cassak‐Shay reconnection‐rate formula at the dayside magnetopause, a numerical factor M is developed to quantify the effect of ρ m on the dayside reconnection rate. It is argued that the mass loading of dayside reconnection by ρ m also makes reconnection more susceptible to shutoff by magnetosheath velocity shear: a formula is developed to estimate the shortening of the dayside reconnection X‐line by ρ m . Surveys of plasmaspheric drainage plumes at geosynchronous orbit during high‐speed‐stream‐driven storms and coronal mass ejection (CME)‐driven storms are presented: in the surveys the CME‐driven storms are separated into sheath‐driven portions and magnetic‐cloud‐driven portions. The storm time mass density of the warm plasma cloak (ionospheric outflows into the electron plasma sheet) is obtained from Alfven‐wave analysis at geosynchronous orbit. A methodology is developed to extrapolate geosynchronous‐orbit plasma measurements to the dayside magnetopause. For each of the three plasmas, estimates of the fractional reduction of the total dayside reconnection rate vary, with typical values of tens of percent; i.e., solar wind/magnetosphere coupling is reduced by tens of percent during storms by oxygen in the ion plasma sheet, by the plasmaspheric drainage plume, and by the plasma cloak. Dependence of the reduction on the F 10.7 solar radio flux is anticipated. Via these ionospheric‐origin plasmas, the magnetosphere can exert some control over solar wind/magnetosphere coupling. Pathways to gain a fuller understanding of the physics of the solar wind‐driven magnetosphere‐ionosphere system are discussed.