Coronal Expansion and Solar Wind |
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¹H+ Alfvén speed Alfvén waves ambient solar wind basic two-fluid model blast wave Burlaga chromosphere Class coronal density coronal expansion coronal expansion models coronal temperature coulomb collisions discussion electron and proton electron temperature emission energy flux density energy source energy-per-charge ergs expansion speed flare ejecta flow speed fluid geomagnetic gradient Hartle heat conduction flux helium helium abundance high-speed plasma streams high-speed streams hydrogen hydrostatic equilibrium implies interplanetary magnetic field interplanetary plasma interplanetary shock waves interplanetary space ionization ions km sec km sec-1 magnetic field lines magnetic sectors one-fluid model particle phenomena photospheric physical polarity post-shock predicted pressure produced propagation proton temperature r=ro radial ratio region scale sec¯¹ sec¹ shock front solar activity solar corona solar flares solar rotation solar wind disturbances solar wind observations solar wind properties solar wind speed solutions source surface spacecraft spectral peak spherically-symmetric steady thermal conductivity variations Vela velocity viscosity