The Solar Wind.pdf

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• In some CMEs there areboth forward and reverseshock.– 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 magnetic
•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 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 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: • The magnetic field configuratio
Page 37: • The Voyager passage through the

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