The Solar Wind.pdf
The Solar Wind.pdf The Solar Wind.pdf
• Until the 1990’s our knowledge of the heliosphere was limited tothe ecliptic.• The 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].– The 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 1 and 2: ESS 200CLectures 6 and 7The Solar W
- Page 3 and 4: • Solar wind speeds (heavy lines)
- Page 5 and 6: • It is useful to describe the so
- Page 8 and 9: • The transition from subsonic to
- Page 10 and 11: • For the solar wind to continue
- Page 12 and 13: • Waves and turbulence?- One poss
- Page 15: • In summary the outer layer of t
- Page 19: ω > Sunv ϕϕSun r r- At large dis
- Page 22: • A meridian view of the IMF- The
- Page 26 and 27: • Observations of high speed stre
- Page 28: • Time series of parameters assoc
- Page 33 and 34: • A coronal mass ejection in spac
- Page 35 and 36: • The magnetic field configuratio
- Page 37 and 38: •The solar wind forms abubble, ca
- Page 39: • The Voyager passage through the
• 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.
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