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New England Space Science Meeting 2: Transition from the Open to Closed Corona

New England Space Science Meeting 2: Transition from the Open to Closed Corona. Nathan Schwadron Jan 4, 2005. Ideas. Where are the transitions Do we see them with TRACE? Source Surface Models .. Which field lines hae opened during CMEs

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New England Space Science Meeting 2: Transition from the Open to Closed Corona

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  1. New England Space Science Meeting 2:Transition from the Open to Closed Corona Nathan Schwadron Jan 4, 2005

  2. Ideas • Where are the transitions • Do we see them with TRACE? • Source Surface Models .. Which field lines hae opened during CMEs • What is the connection between a region with open field and a region that appears dark in a particular band?

  3. Welcome • Purpose: • To facilitate interaction among colleagues in space science in the New England Area (UNH, CfA, BU, MIT, Hanscom/AFRL, Haystack, Dartmouth) • To leverage these interactions for initiating new, cross-disciplinary and far-reaching projects • Meetings: • Monthly meetings (first wed each month) • Workshop?

  4. Relationship of open and closed field topologies • Potential field models (static) • Role of time-dependency (continuous transitions from open to closed states?) • Conservation of open magnetic flux • Is open flux conserved, or just preserved • Highly sectored open fields vs structured closed fields • Open field reflects dipole term • Closed fields on much smaller scales

  5. Relationship of solar wind and coronal heating • Open field regions free to form steady (supersonic) flows • Closed field regions injected energy largely lost through radiation • Is a transition between these regimes expected?

  6. Paths for Deposited Coronal Energy Injected Electromagnetic Energy Bound, closed structures Transition ?? Open field Downward Conducted Heat, Radiation, Siphon flows Slow wind Fast wind Hot & Bright Intermediate? Fluctuating? Cool & Dark

  7. Paths of deposited Energy • Solar Wind Scaling Law • Electron heat conduction and radiative losses Fast wind Cool, Dark Slow wind Warm,Brighter Radiative Loss Hot, Bright Schwadron and McComas, ApJ, 2003

  8. Background Well known anti-correlation between solar wind speed and freezing-in temperature, low FIP elements (Geiss et al, Science, 1995; von Steiger et al., JGR, 2000, Gloeckler, et al. 2003) von Steiger et al., JGR, 2000

  9. Constant Energy/particle Source Schwadron and McComas, ApJ, 2003

  10. Flux-Flux Scaling Injected Elec.Mag. Energy/Particle (assumed constant) Constant injected energy/particle implies injected power proportional to particle flux and magnetic flux: Injected Power proportional to magnetic flux

  11. From Solar Wind to X-rays • Solar wind power • Yohkoh (2.8-36.6 Å) Lx~ 1-2% Pcorona ~ 500 0 ??

  12. T-Tauri Stars G,K,M dwarfs Solar Wind Disk Averages Active Regions X-ray Bright Points Quiet Sun Solar Wind to X-rays, Lx = 500 0 Pevstov et al., 2003, Schwadron et al., 2005

  13. X-rays over the Solar Cycle Schwadron et al., 2005 Power proportional To Magnetic Flux

  14. X-rays over the solar cycle • Solar Wind Power • GOES (1-8 Å) Active Regions: Lx~ 2.5x10-4 Pcorona Quiet Regions: Lx~ 5x10-5 Pcorona Coronal Holes: Lx~9x10-10 Pcorona

  15. Solar Minimum vs Solar Max McComas et al., GRL, 2003 Solar wind’s high degree of organization by speed

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