Thermosphere-Ionosphere Issues for DASI - I:

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Presentation transcript:

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

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

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)

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

Tidal Coupling into the Low & Middle Latitude Daytime Ionosphere E-region Dynamo ~90-160 km charge separation: electrons gyrate along B ions move across B with neutrals polarization electric field maps up into the F-region

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

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

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?

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

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

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

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

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

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