The Solar Wind.pdf

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• For the solar wind to continue to accelerate then themean thermal energy must exceed the gravitationalenergy.• To have a solar wind a star must have a cool loweratmosphere and a hot outer atmosphere.• How is the corona heated?−γp ρ = const.cp– Assume an ideal gas where γ = = ratio ofcvspecific heats.– If there is no heat gain or loss then the system is adiabatic5and γ =32 γ p– c s=ρGMSun 2– Taking the spatial derivative of > 2cswe findrd 20 > csrdrd γ −10 > ( rρ )dr
• Solvingρ ⎛> ⎜ρ ⎝0r0r⎞⎟⎠1γ −1Where ρ is the density at the base of the atmosphere r 0 .0• From the conservation of mass we getρ ⎛ r< ⎜ρ ⎝ r• <strong>The</strong>se two conditions cannot be solved for3and thereforethe lower atmosphere can’t be adiabatic.• Heat must be supplied from the cooler stellar surface!00⎞⎟⎠2γ =5
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 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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