Particle “Precipitation” in the Thermosphere / Ionosphere1 Particle “Precipitation” in the...
Transcript of Particle “Precipitation” in the Thermosphere / Ionosphere1 Particle “Precipitation” in the...
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Particle “Precipitation”in the
Thermosphere / Ionosphere
Stan SolomonHigh Altitude Observatory
National Center for Atmospheric Research
HEPPA 2009 • Center Green • 6 October 2009
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What “Precipitation” Affects the Thermosphere/Ionosphere
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Primarily auroral electrons in the energy range 100 eV – 100 keV...also protons and other ions in the energy range 1 keV – 1 MeV
Radiation belt particles, Solar energetic particles, cosmic rays, etc., are of little importance above ~90 km, because they pass right through the thermosphere.
“I got no kick against the east coast; you know the people there have got the most; and New York City’s like a friendly ghost, you seem to pass right through...” — Bob Segar, Katmandu.
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Outline of Presentation
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• Simple tutorial on auroral energy deposition and thermosphere/ionosphere effects
• Introduction to the odd-nitrogen problem and the sources of nitric oxide
• Integrated auroral power and the magnitude of the chemical response
...not going to talk about:
— electrodynamical coupling and Joule heating
— disruption of the ionospheric electric field
— response of thermospheric temperature, density, and wind
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Reconnection in the Magnetotail
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Coupled Magnetosphere-Ionosphere-Thermosphere Model
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Energetic Particles from the Magnetosphere
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Motion of Charged Particles Along a Magnetic Field Line
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Transport of Auroral Electrons in the Upper Atmosphere
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Penetration Depth of Auroral Electrons Depends on Energy
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Thermosphere and Ionosphere Composition
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Auroral Collisional Processes
Electron Impact Ionization
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Ion Recombination Processes
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Examples of Auroral Emission Processes
Molecular Nitrogen:
e* + N2 → 2e* + N2+(B2Σu
+) N2+(B2Σu
+) → N2+(X1Σg
+) + hν (1N bands)
e* + N2 → e* + N2(B3Πg) N2(B3Πg) → N2(X1Σg+) + hν (1P bands)
e* + N2 → e* + N2(A3Σu+) N2 (A3Σu
+) → N2(X1Σg+) + hν (VK bands)
N2 (A3Σu+) + O(3P) → N2(X1Σg
+) + O(1S)
O(1S) → O(3P) + hν (5577Å)
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Examples of Auroral Emission Processes
Atomic Oxygen:
e* + N2 → e* + N2(A3Σu+) N2 (A3Σu
+) + O(3P) → N2(X1Σg+) + O(1S)
O(1S) → O(3P) + hν (5577Å) τ~1s
e* + O(3P) → e* + O(1S) O(1S) → O(3P) + hν (5577Å) τ~1s
e* + O(3P) → e* + O(1D) O(1D) → O(3P) + hν (6300Å) τ~100s
O2+ + e- → O + O(1D) O(1D) → O(3P) + hν (6300Å) τ~100s
O(1D) + N2 → O(3P) + N2
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Examples of Auroral Emission Processes
Atomic Nitrogen:
e* + N2 → e* + N(4S) + N(2D) N(2D) → N(4S) + hν (5200Å) τ~100,000s
N(2D) + O → N(4S) + O
NO+ + e- → O + N(2D) N(2D) → N(4S) + hν (5200Å) τ~100,000s
N(2D) + O → N(4S) + O
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Simplified Schematic of Ion-Neutral Chemistry
Ionization leads inexorably to dissociation
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Simplified Schematic of E-region Ion-Neutral Chemistry
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Simplified Schematic of Odd-Nitrogen Chemistry
N2
N(2D)
NO
N(4S)
O
O2
N2
e*, hν
N(4S)
O2
NO
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Measurements of Nitric Oxide by SNOE
Thermospheric NO Peak Density at 107 km, Day 1998 070
SNOE measured thermospheric nitric oxide using γ-band fluorescence method.Measurement constrained to sunlit locations (i.e., can’t measure at winter pole)
Altitude range 90–170 km; best quality data in range 100–150 km
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Measurements of Nitric Oxide by SNOEDaily mean data at ~11 AM local solar time (15 orbits) averaged over all longitudes
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Comparison of SNOE NO to TIE-GCM 1.8 CalculationsSNOE TIE-GCM
Equinox
Solstice
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Comparison of SNOE NO to TIE-GCM 1.8 CalculationsSNOE TIE-GCM
LowAurora
HighAurora
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The 80’s View — Linear Fit to NOAA/DMSP Particle Data
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...But More Recent NOAA/DMSP HP Estimates are Higher
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Fit to Current HP Estimates is Approximately 2 x Maeda
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Comparison to HP Integrated over the “Hardy Oval”
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Auroral Measurements by the TIMEDGlobal Ultraviolet Imager (GUVI)
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GUVI Empirical Auroral Oval(ongoing work by Yongliang Zhang, Wenbin Wang, Xiaoli Luan)
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Comparison to New Estimates from TIMED/GUVI
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Morphology of Some Empirical Auroral Ovals
Kp=2
Kp=4
Kp=6
NOAA GUVI Hardy TIE-GCM
mW m-2
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Nitric Oxide in NCAR General Circulation Models
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Where we are:
— Believe that we have a realistic representation of auroral distribution and HP...also now parameterized using solar wind / IMF input
— But TIE-GCM v. 1.93 still doesn’t produce quite enough nitric oxide...especially during high auroral activity
— Still get reasonable agreement with SNOE general morphology...including latitudinal, seasonal, and solar cycle dependence
— Also get good agreement with SABER cooling rate observations...see talk by Mlynczak et al., later this afternoon.
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