The Slow Solar Wind Tom Holzer NCAR/HAO NCAR/HAO.

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Presentation transcript:

The Slow Solar Wind Tom Holzer NCAR/HAO NCAR/HAO

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

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

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

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

Observational Constraints—3 In situ observations of elemental abundance and ionization state (Neugebauer, Tues. PM) 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)

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

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

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

Subsonic Momentum Balance (Steady State) Effective Pressure & Gravitational Escape Speed Asymptotic Flow Speed Mass Flux, Energy Flux, and Asymptotic Flow Speed—2

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

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

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

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

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

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

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

Types of Slow Solar Wind Models Transient ejection of wind from magnetically closed regions (Dahlburg, Wed. AM) Endeve et al., 2003

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

Interaction of Observation and Theory Each theory should be compared with all relevant observations Each observation should be compared with all relevant theories

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)