The Solar Wind.pdf

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• Until the 1990’s our knowledge of the heliosphere was limited tothe ecliptic.• <strong>The</strong> Ulysses spacecraft observed the flow over both thenorthern and southern poles of the Sun.• No latitudinal gradient in B r .– Magnetic flux is removed from the poles toward the equatorialregions.– Sketch showing equatorial current sheet and magnetic field linescoming from the polar regions toward the equator. [Smith et al.,1978]
• Plasma measurementsshow a dramatic change invelocity with latitude inobservations takenbetween 1992 and 1997.[McComas et al., 1998].– <strong>The</strong> velocity increases fromabout 450 km/s at theequator to about 750 km/sabove the poles.– Above 50 0 only fast solarwinds streaming out ofcoronal holes were observed.– Up to about 30 0 a recurrentCIR was observed with aperiod of about 26 days.
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 and 22: • That the IMF has sector structu
Page 23 and 24: • The solar wind speed and densit
Page 25 and 26: • The Archimedean spiral associat
Page 27: • Changes in the solar wind plasm
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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