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1 K. Stasiewicz, Plasma Space Science Center, NCKU Swedish Institute of Space Physics, Uppsala Multi-spacecraft studies of nonlinear waves
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2 Turbulence in the foreshock
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3 Shocklets in the foreshock
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4 Fast solitons in the foreshock
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5 mirror structures (shifted timeseries)
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6 Propagating mirror modes (holes)
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7 Multi-point measurements by Cluster: velocity determination R 21 V sn
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8 Magnetosonic solitons: observations and model Stasiewicz, Shukla, …et al, Phys. Rev. Lett. 90, 085002 (2003)
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9 Convergent E structure negative potential Divergent E structure positive potential Auroral acceleration structures (alfvenons) as solutions of two-fluid equations
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10 How particles are accelerated?.... by electric fields only, but
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11 Auroral acceleration structures: negative or positive potentials 10-20 keV
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12 Acceleration/heating in the solar corona Flares acceleration potentials ~10-1000 kV Solar wind: 600 km/s escape velocity + 300-800 km/s equivalent: 2-5 kV Heating: (millions K) 5 MK equivalent: 0.5 kV
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13 Two fluid equations for ions j=i and electrons j=e Can be reduced to ion momentum equation And the generalized Ohm’s law Two-fluid equations
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14 Soliton solutions
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15 Dispersion diagram for slow alfvenons
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16 THE END www.cluster.irfu/ks/
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