The Solar Wind.pdf

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• The transition from subsonic to supersonic occurs at a criticalradius r c where v = c s• In order for a real continuous solution to exist at r cGMSunrc=22cs• The form of solutions for the expansion of the solar wind• Solution A is the “observed” solar wind. It starts as a subsonicflow in the lower corona and accelerates with increasing radius.At the critical point the solar wind becomes supersonic.• For solution F the speed increases only weakly with height andthe critical velocity is not reached. For this case the solar wind isa “solar breeze”.• For solution C the flow accelerates too fast, becomessupersonic before reaching the critical radius and turns aroundand flows into the Sun.
• Solution B starts as a supersonic flow in the lower corona andbecomes subsonic at the critical point.• If the flow decelerates less as in D it would still be supersonic atthe critical point and be accelerated again.• Solution E is an inward blowing wind that is subsonic. The flowaccelerates as it approaches the Sun, turns back and leaves theSun supersonically.• Quantitative solutions (after Parker [1958])
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 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 31 and 32: • Plasma measurementsshow a drama
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

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