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The Slow Solar Wind Tom Holzer NCAR/HAO NCAR/HAO
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Topics to be Discussed Mass flux, energy flux, and asymptotic flow speed Physical ingredients for a slow solar wind Observational constraints on slow solar wind models Types of slow solar wind models Interaction of observation and theory
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Topics to be Discussed Mass flux, energy flux, and asymptotic flow speed Physical ingredients for a slow solar wind Observational constraints on slow solar wind models Types of slow solar wind models Interaction of observation and theory
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Observational Constraints—1 In situ observations: n, u, B, T, q, elemental abundance & ionization state (Neugebauer, Tues. PM) Mapping back to the Sun Comparison with disk and limb solar observations (also radio) YOHKOH & HAO Hundhausen, 1980 Inferredmagnetic neutral line Carrington rotation 1610 (early 1974) Recurrentgeomagneticactivity(mapped) Solar wind speed and magneticpolarity(mapped) Coronalpolarizationbrightness Coronal x-ray emission 1 R sun 3 R sun 1.5 R sun 1 AU
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Observational Constraints—2 Off-limb and on-disk spectral and filter observations (Feldman, Raymond, Tues. PM) SOHO/UVCS O VI H I Si XII C III Fe XVIII Mg X: SOHO/SUMER O IV: SOHO/CDS Fe XII: SOHO/EIT
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Observational Constraints—3 In situ observations of elemental abundance and ionization state (Neugebauer, Tues. PM) 10 2 10 7 10 3 10 4 10 5 10 6 12345678910 Radial Distance (R sun ) Characteristic Time (s) Equilibration Time Expansion Time Freezing in of the ionization state for O +6 and O +7 (Owocki, 1982) Solar wind speed and coronal electron temperature (Gloeckler et al., 2003)
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Observational Constraints—4 Photospheric magnetic field observations with source-surface, potential-field extrapolation Wang-Sheeley-Arge (WSA) approach: No talk scheduled Arge & Pizzo (2000) Source Surface Speed Expansion Factor
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Topics to be Discussed Mass flux, energy flux, and asymptotic flow speed Physical ingredients for a slow solar wind Observational constraints on slow solar wind models Types of slow solar wind models Interaction of observation and theory
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Mass Flux, Energy Flux, and Asymptotic Flow Speed—1 Corona/Wind Energy Balance (Steady State) Flow Energy Flux Constant Mass Flux Total Energy Flux Large Distances Coronal Base Downward Conduction Flux Enthalpy Flux Conduction Flux Gravitational Potential Energy Flux Wave
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Subsonic Momentum Balance (Steady State) Effective Pressure & Gravitational Escape Speed Asymptotic Flow Speed Mass Flux, Energy Flux, and Asymptotic Flow Speed—2
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Mass Flux, Energy Flux, and Asymptotic Flow Speed—3 Critical Point Density Mass Flux Mass flux increases with increasing temperature and expansion factor Chromosphere-corona coupling is crucial (Rosner et al., 1976; Hansteen & Leer, 1995) Hansteen & Leer, 1995) upward enthalpy flux
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Topics to be Discussed Mass flux, energy flux, and asymptotic flow speed Physical ingredients for a slow solar wind Observational constraints on slow solar wind models Types of slow solar wind models Interaction of observation and theory
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Physical Ingredients for a Slow Solar Wind Asymptotic Flow Speed Subsonic Heating (i.e., increasing T) Subsonic Flow Tube Expansion (increase) Increased mass flux decreased asymptotic flow speed
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Topics to be Discussed Mass flux, energy flux, and asymptotic flow speed Physical ingredients for a slow solar wind Observational constraints on slow solar wind models Types of slow solar wind models Interaction of observation and theory
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Types of Slow Solar Wind Models Wind from quasi-steady open magnetic geometries Wind from reconnecting open and closed field lines Transient ejection of wind from magnetically closed regions
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Types of Slow Solar Wind Models Wind from quasi-steady open magnetic geometries Chromosphere-corona coupling is crucial Ofman (slow wind), Hollweg (fast wind)—Wed. AM) Hundhausen, 1980
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Types of Slow Solar Wind Models Wind from reconnecting open and closed field lines No talk scheduled, but ask Len Fisk—Wed. AM Fisk (2003) Closed-closedreconnection Open-closedreconnection Old Open Field Line New Open Field Line
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Types of Slow Solar Wind Models Transient ejection of wind from magnetically closed regions (Dahlburg, Wed. AM) Endeve et al., 2003
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Topics to be Discussed Mass flux, energy flux, and asymptotic flow speed Physical ingredients for a slow solar wind Observational constraints on slow solar wind models Types of slow solar wind models Interaction of observation and theory
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Interaction of Observation and Theory Each theory should be compared with all relevant observations Each observation should be compared with all relevant theories
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Potential Field Extrapolation Pneuman & Kopp (1971) Solid lines: isothermal mhd simulation with dipole lower boundary condition with dipole lower boundary condition Dashed lines: potential field source surface model with same b.c. surface model with same b.c. Near the streamer, f ss is larger for the PFSS model than for the MHD model Newkirk (1972)
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