1. Thermosphere-Ionosphere Issues for DASI - I:
Quiescent Variability
what are the magnitudes & sources of global quiescent thermosphere-ionosphere (TI) variations?
does the quiescent global variability “pre”condition the TI response to space weather events?
Diagnostic Wish List
global Tn, Un, Vn, r, Ne, Ti, Ui, Vi, Wi, DH, DD, DZ, (?)
leverage all ground-based & space-borne measurements
correlative analyses to quantify wave signatures
DASI Deployment Strategies
develop/assess data assimilation models (e.g., GAIM; GSWM-DA); use DA to quantify optimum data requirements (quality-location-cadence) for fielding new instruments
correlative/interpretive numerical modeling efforts

2. partially transparent
opaque
transparent
partially transparent
Courtesy of Judith Lean (NRL)

3. Solar FUV & EUV Energy Deposition in the Earth’s Upper Atmosphere
Solar Cycle Minimum
Solar Cycle Maximum
EUV variations of ~30% 
variable thermospheric heating
variable thermospheric density
variable satellite drag
Courtesy of Stan Solomon (HAO)

4. TIE-GCM Results LBC: GSWM-02 Tides Zonal Wind (m/s) near 120km

5. Tidal Coupling into the Low & Middle Latitude Daytime Ionosphere
E-region Dynamo
~ km
charge separation:
electrons gyrate along B
ions move across B with
neutrals
polarization electric field
maps up into the F-region

6. Natural Variability of the Quiescent Ionosphere (after Mendillo et al
daily
predictions
coupled
CCM3
TIME-
GCM
39oN
52oN
45oN
peak density
vs. UT
1s:
monthly
mean
ionosonde
data
52oS
28oS
43oS

7. Macro-Scale Effects of Micro- & Meso-Scale Variations
The TI Gateway: The Mesopause Region
Gravity Waves:
sources,
evolution,
dissipation,
effects
???? penetration
into the TI

8. Thermosphere-Ionosphere Issues for DASI - II:
The TI during Space Weather Events – Tracing the Energy Deposition and the Thermal, Dynamical, and Chemical TI Effects
how does the global TI respond to geomagnetic storms?
how does the global response vary with altitude?
how does the global response vary with time?
what are the local responses to Solar Proton Events (SPEs)?
do SPEs produce a global response?
how deep into the atmosphere do the local and global effects penetrate?
how does the thermosphere affect the ionosphere?…the magnetosphere?

10. Zonal Mean Auroral Energy Input
Heating Efficiency: ~30%
April 17,2002
upper thermosphere
~250 km
~150 km
lower thermosphere
~110 km*
mesopause region
~90 km
mW/m2

11. Northern Hemispheric Warming near 110 km
April 17 UT=0 ….before major onset
Nitric Oxide Density Enhancements
Auroral Energy Flux  
+++ dynamics +++
Auroral Heating  
Radiational Cooling Changes 
temperature

12. Northern Hemispheric Warming near 110 km
April 17 UT=20 ….during major storm
Nitric Oxide Density Enhancements
Auroral Energy Flux  
+++ dynamics +++
Auroral Heating  
Radiational Cooling Changes 
temperature

14. GOES-8 Proton Flux April 21-23, 2002 Produce NOx & HOx  Affects O3
mesosphere
Produce NOx & HOx
 Affects O3
stratosphere

15. TIME-GCM Ionization Rates over Antarctica
…with-without solar protons 

16. Composition Changes over Antarctica
…from TIME-GCM results with & without solar protons
% change [NO+NO2] 
deeper and longer-lived
% change [O3]