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The plasma number density in the near-Earth plasma sheet depends on the\udsolar wind number density and the north-south component of interplanetary\udmagnetic field (IMF Bz) with time lag and duration of several hours. We\udexamined the three-dimensional structure of such dependences by fitting\udobservations of plasma sheet and solar wind to an empirical model equation.\udAnalyses were conducted separately for northward and southward IMF\udconditions. Effects of solar wind speed and IMF orientation were also\udexamined by further subdivision of the dataset. Based on obtained results,\udwe discuss (i) the relative contribution of the ionosphere and solar wind to\udplasma sheet mass supply, (ii) the entry mechanisms for magnetosheath\udparticles, and (iii) the plasma transport in the plasma sheet. We found that\udsolar wind number density dependence is weaker and IMF Bz dependence is\udstronger for faster solar wind with southward IMF, which suggests the\udcontribution of ionospheric particles. Further from the Earth, different\udinterplanetary conditions result in different structures of solar wind\uddependence, which indicate different solar wind entry mechanisms: (1)\udsouthward IMF results in a strong dependence on solar wind number density in\udthe flank high-latitude region, (2) slow solar wind with northward IMF leads\udto lower-latitude peaks of solar wind number density dependence in the flank\udregion, (3) fast solar wind with northward IMF results in a strong\uddependence on solar wind number density at the down-tail dusk flank equator,\udand (4) solar wind number density dependence is stronger in the downstream\udof quasi-parallel bow shock. These features are attributable to (1)\udlow-latitude dayside reconnection entry, (2) high-latitude dayside\udreconnection entry, (3) entry due to decay of Kelvin-Helmholtz vortices, and\ud(4) diffusive entry mediated by kinetic Alfven waves, respectively. Effect\udof IMF Bz and its time lags show plasma sheet reconfiguration associated\udwith enhanced convective transport under southward IMF. Duration of IMF Bz\udeffect under northward IMF is interpreted in terms of turbulent diffusive\udtransport

Solar wind control of plasma number density in the near-Earth plasma sheet: three-dimensional structure