The Solar Wind.pdf

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• The IMF can be directed either inward or outwardwith respect to the Sun.• One of the most remarkable observations from earlyspace exploration was that the magnetic field polaritywas uniform over large angular regions and thenabruptly changed polarity.– This polarity pattern repeated over succeeding solarrotations. The regions of one polarity are called magneticsectors.– In a stationary frame of reference the sectors rotate with theSun.– Typically there are about four sectors.– The sector structure gets very complicated during solarmaximum.
• The sector structure inferred from IMP satelliteobservations. Plus signs are away from the Sun andminus signs are toward the Sun.
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: ω > Sunv ϕϕSun r r- At large dis
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 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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