The Solar Wind.pdf

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• In some CMEs there areboth forward and reverseshocks.– The forward shock forms in theslow solar wind speeding it uprelative to the Earth, but slowingthe flow as seen by the CME.– The reverse shock propagatesinto the magnetic cloud slowing itdown relative to the Earth.• The cloud may be rotated anany angle about the Earth-Sunline.• How long the cloud staysconnected to the Sun is notknown.• Magnetic clouds are the maincause of geomagneticdisturbances called magneticstorms at Earth.
•The solar wind forms abubble, called the heliosphere,in the partially ionized localinterstellar medium (LISM).•We do not know if the LISM issubsonic – the LISM flow willbe diverted around theheliospheric obstacle eitheradiabatically or by forming abow shock.•The boundary separating theheliosphere from the LISM isthe heliopause (HP).•The solar wind is supersonicand a shock (the terminationshock-TS) forms within theheliosphere as it approachesthe heliopause.•The region of shockedplasma between the TS andthe heliopause is called theinner heliosheath.•In the simulation below theLISM flow was assumed tobe supersonic and nointerstellar neutral hydrogenwas assumed.Contours of temperature andflow streamlines- from Zank etal., 2001
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 31 and 32: • Plasma measurementsshow a drama
Page 33 and 34: • A coronal mass ejection in spac
Page 35: • The magnetic field configuratio
Page 39: • The Voyager passage through the

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