Not listed THE SOLAR CORONA AND SOLAR WIND EXHIBIT TURBULENCE WHICH IS BELIEVED TO PLAY AN IMPORTANT ROLE IN GLOBAL HELIOSPHERIC DYNAMICS HEATING THE SOLAR CORONA AND ACCELERATING AND CONTINUOUSLY HEATING THE SOLAR WIND. AS THE SOLAR WIND FLUCTUATIONS CASCADE TO SMALLER AND SMALLER SCALES THEY BECOME STRONGLY ANISOTROPIC WITH MOST ENERGY CONCENTRATED IN VARIATIONS PERPENDICULAR TO THE MAGNETIC FIELD. MANY TURBULENCE STUDIES CHARACTERIZE THIS TURBULENCE AS ALFVENIC FLUCTUATIONS BECOMING KINETIC ALFVEN WAVES AT SUB-MHD SCALES. HOWEVER THE SOLAR WIND IS FILLED WITH OTHER DYNAMICS BEYOND THESE MODELS E.G. SMALL-SCALE TRANSIENT STRUCTURES SUCH AS MAGNETOSONIC AND WHISTLER FLUCTUATIONS ARE A FREQUENT OCCURRENCE. 0$ 4/28/21 P00002 THE SOLAR CORONA AND SOLAR WIND EXHIBIT TURBULENCE WHICH IS BELIEVED TO PLAY AN IMPORTANT ROLE IN GLOBAL HELIOSPHERIC DYNAMICS, HEATING THE SOLAR CORONA AND ACCELERATING AND CONTINUOUSLY HEATING THE SOLAR WIND. AS THE SOLAR WIND FLUCTUATIONS CASCADE TO SMALLER AND SMALLER SCALES, THEY BECOME STRONGLY ANISOTROPIC, WITH MOST ENERGY CONCENTRATED IN VARIATIONS PERPENDICULAR TO THE MAGNETIC FIELD. MANY TURBULENCE STUDIES CHARACTERIZE THIS TURBULENCE AS ALFVENIC FLUCTUATIONS BECOMING KINETIC ALFVEN WAVES AT SUB-MHD SCALES. HOWEVER, THE SOLAR WIND IS FILLED WITH OTHER DYNAMICS BEYOND THESE MODELS, E.G., SMALL-SCALE TRANSIENT STRUCTURES SUCH AS MAGNETOSONIC AND WHISTLER FLUCTUATIONS ARE A FREQUENT OCCURRENCE. Funding Only Action 0$ 4/28/21 P00001 THE SOLAR CORONA AND SOLAR WIND EXHIBIT TURBULENCE WHICH IS BELIEVED TO PLAY AN IMPORTANT ROLE IN GLOBAL HELIOSPHERIC DYNAMICS, HEATING THE SOLAR CORONA AND ACCELERATING AND CONTINUOUSLY HEATING THE SOLAR WIND. AS THE SOLAR WIND FLUCTUATIONS CASCADE TO SMALLER AND SMALLER SCALES, THEY BECOME STRONGLY ANISOTROPIC, WITH MOST ENERGY CONCENTRATED IN VARIATIONS PERPENDICULAR TO THE MAGNETIC FIELD. MANY TURBULENCE STUDIES CHARACTERIZE THIS TURBULENCE AS ALFVENIC FLUCTUATIONS BECOMING KINETIC ALFVEN WAVES AT SUB-MHD SCALES. HOWEVER, THE SOLAR WIND IS FILLED WITH OTHER DYNAMICS BEYOND THESE MODELS, E.G., SMALL-SCALE TRANSIENT STRUCTURES SUCH AS MAGNETOSONIC AND WHISTLER FLUCTUATIONS ARE A FREQUENT OCCURRENCE. Other Administrative Action $0 9/9/20 Not listed THE SOLAR CORONA AND SOLAR WIND EXHIBIT TURBULENCE WHICH IS BELIEVED TO PLAY AN IMPORTANT ROLE IN GLOBAL HELIOSPHERIC DYNAMICS HEATING THE SOLAR CORONA AND ACCELERATING AND CONTINUOUSLY HEATING THE SOLAR WIND. AS THE SOLAR WIND FLUCTUATIONS CASCADE TO SMALLER AND SMALLER SCALES THEY BECOME STRONGLY ANISOTROPIC WITH MOST ENERGY CONCENTRATED IN VARIATIONS PERPENDICULAR TO THE MAGNETIC FIELD. MANY TURBULENCE STUDIES CHARACTERIZE THIS TURBULENCE AS ALFVENIC FLUCTUATIONS BECOMING KINETIC ALFVEN WAVES AT SUB-MHD SCALES. HOWEVER THE SOLAR WIND IS FILLED WITH OTHER DYNAMICS BEYOND THESE MODELS E.G. SMALL-SCALE TRANSIENT STRUCTURES SUCH AS MAGNETOSONIC AND WHISTLER FLUCTUATIONS ARE A FREQUENT OCCURRENCE. $0 9/9/20 Not listed THE SOLAR CORONA AND SOLAR WIND EXHIBIT TURBULENCE WHICH IS BELIEVED TO PLAY AN IMPORTANT ROLE IN GLOBAL HELIOSPHERIC DYNAMICS HEATING THE SOLAR CORONA AND ACCELERATING AND CONTINUOUSLY HEATING THE SOLAR WIND. AS THE SOLAR WIND FLUCTUATIONS CASCADE $97.8k 9/20/19