The Solar Wind.pdf

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• As the Sun rotates the three dimensional currentsheet becomes wavy. This is sometimes called theBallerina skirt model of the heliosphere.
• The solar wind speed and density have large variations ontime scales of days. Of special interest are high speedstreams.– The flow speed varies from pre-stream levels (400 km/s) reaching amaximum value (600 km/s – 700 km/s) in about one day.– The density rises to high values (>50 cm -3 ) near the leading edgesof the streams and these high densities generally persist for about aday. The peaks are followed by low densities lasting several days.– The proton temperature varies like the flow speed.– The high speed streams tend to have a dominant magnetic polarity.– The dominant source of high speed streams is thought to be fieldlines that are open to interplanetary space. These regions areknown as coronal holes.
Page 6: • The solar wind exists because t
Page 9 and 10: • Solution B starts as a superson
Page 11 and 12: • Solvingρ ⎛> ⎜ρ ⎝0r0r⎞
Page 13 and 14: • In summary the outer layer of t
Page 15 and 16: • Assume a plasma parcel on the S
Page 17 and 18: ω > Sunv ϕϕSun r r- At large dis
Page 19 and 20: • The sector structure inferred f
Page 21: • That the IMF has sector structu
Page 25 and 26: • The Archimedean spiral associat
Page 27 and 28: • Changes in the solar wind plasm
Page 29 and 30: • Plasma measurementsshow a drama
Page 31 and 32: • A coronal mass ejection in spac
Page 33 and 34: • The magnetic field configuratio
Page 35 and 36: •The solar wind forms abubble, ca
Page 37: • The Voyager passage through the

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