Long Term Observations of Earth s Upper Atmosphere
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1 Long Term Observations of Earth s Upper Atmosphere SME UARS Aura EnviSat TIMED Nimbus VII Marty Mlynczak NASA Langley Research Center SORCE 11/20/2015 Sun-Climate Symposium
2 Outline The golden age of upper atmospheric science Some long-term observations in the stratosphere, mesosphere, and thermosphere After 40 years, what s there left to do? The Atmospheric Coupling Explorer Mission Summary 11/20/2015 Sun-Climate Symposium
3 The Golden Age of Upper Atmospheric Science Concerns over the ozone layer prompted development of satellite measurement of ozone, thermal structure, related chemistry, and dynamics Experimental techniques involve both limb and nadir observations Limb sensors for both solar occultation and thermal emission Nadir sensors for backscatter ultraviolet (e.g. SBUV, TOMS) Multiple U. S. and International instruments and missions flown over past 40 years to understand stratosphere, mesosphere, and lower thermosphere/ionosphere 11/20/2015 Sun-Climate Symposium
4 Upper Atmosphere Satellite Instruments and Missions 1970 s -- LRIR, LIMS, AE, SAM 1980 s -- DE-1, DE-2, SAGE-II, SME 1990 s -- UARS, POAM 2000 s -- Aura, TIMED, Envisat, ODIN, SciSat, SAGE-III, SORCE, SMILES, AIM 2010 s -- SAGE III (2016); ICON; GOLD UARS AURA 2020 s --???? No missions in preparation for middle atmosphere science Eniat 11/20/2015 Sun-Climate Symposium
5 Upper Atmosphere Satellite Instruments and Missions 1970 s -- LRIR, LIMS, AE, SAM 1980 s -- DE-1, DE-2, SAGE-II, SME 1990 s -- UARS, POAM 2000 s -- Aura, TIMED, Envisat, ODIN, SciSat, SAGE-III, SORCE, SMILES, AIM 2010 s -- SAGE III (2016); ICON; GOLD UARS AURA 2020 s --???? No missions in preparation for middle atmosphere science Eniat A gap in thermal structure and chemical composition measurements after 2020 seems inevitable 11/20/2015 Sun-Climate Symposium
6 Selected Long-Term Observations Stratospheric Temperature Mesospheric Carbon Dioxide Thermospheric Infrared Radiation 11/20/2015 Sun-Climate Symposium
7 Stratospheric Temperature Change: Stratopause is ~ 9 K colder today than in /20/2015 Sun-Climate Symposium
8 Stratospheric Temperature Differences SC 23 Max SC 23 Min SC 24 Max Mlynczak et al, GRL, in prep. 11/20/2015 Sun-Climate Symposium
9 Upper Mesosphere and Lower Thermosphere CO 2 M - L 80 km 90 km 100 km CO 2 trends are not consistent with model predictions Yue et al., GRL, /20/2015 Sun-Climate Symposium
10 Global Radiative Cooling by CO 2 (W) 100 km to 140 km : 5000 days of data Radiative cooling responds on timescales from few days to decades Mlynczak et al., 2003, 2005, /20/2015 Sun-Climate Symposium
11 Global Radiative Cooling by CO 2 (W) 100 km to 140 km : 5000 days of data Comparing Solar Maxima -- DE = 3.5 x Joules 11/20/2015 Sun-Climate Symposium
12 Global Radiative Cooling by NO (W) 100 km to 140 km : 5000 days of data Halloween 2003 St. Pat s 2015 Variability from daily to decadal scale Due to combination of solar UV and geomagnetic variablity 11/20/2015 Sun-Climate Symposium
13 Global Radiative Cooling by NO (W) 100 km to 140 km : 5000 days of data Comparing Solar Maxima -- DE = 3.5 x Joules Mlynczak et al., 2003, 2005, /20/2015 Sun-Climate Symposium
14 Q: After 40 years, what s left to do? A: Understand in detail the explore the region between 100 and 200 km altitude Q. Why? A. Understanding the evolution of entire atmosphere above depends on it 11/20/2015 Sun-Climate Symposium
15 Thermospheric IR Cooling by NO and CO 2 CO 2 cooling dominant below 120 km And at all altitudes during solar minimum Mlynczak et al., JGR, /20/2015 Sun-Climate Symposium
16 Global Cooling due to Increasing CO 2 Roble and Dickinson, 1989 How does increasing CO 2 cool the atmosphere above 140 km? 11/20/2015 Sun-Climate Symposium
17 Altitude (km) Overview of Energy Budget of Atmosphere above 100 km External Energy Input Solar UV Solar Wind 500 Energy Redistribution Heat Conduction Energy Loss 300 Quiet Sun Active Sun NO (5.3 mm) 100 Tides, Waves Temperature (K) CO 2 (15 mm) 11/20/2015 Sun-Climate Symposium
18 Altitude (km) The km Region is the Heat Sink for the Thermosphere External Energy Input Solar UV Solar Wind 500 Energy Redistribution Heat Conduction Energy Loss 300 Quiet Sun Active Sun NO (5.3 mm) 100 Tides, Waves Temperature (K) CO 2 (15 mm) 11/20/2015 Sun-Climate Symposium
19 Atmosphere Coupling Explorer Mission ACE is a mission to explore the thermosphere above 100 km ACE will continue legacy measurements from SABER TLS Instrument (S. Yee, APL) T, O, winds 100 to 160 km 15 kg 25 W MASTER Instrument 35 kg, 35 W 100% SABER Heritage ½ mass, ½ power, 1/3 volume Identical radiometric performance 11/20/2015 Sun-Climate Symposium
20 Altitude (km) Existing Capability CO 2, NO Cooling T O 3 CO 2 H 2 O O /20/2015 Sun-Climate Symposium
21 Altitude (km) 250 Existing Capability ACE Mission Capability Heat Cond. 200 CO 2, NO Cooling T NO O O-Cool CO 2, NO Cooling T O 3 CO 2 H 2 O O NO+ 50 CO 2 CO 15 11/20/2015 Sun-Climate Symposium
22 Summary Long, illustrious history of observations of Earth s stratosphere, mesosphere, and thermosphere Presently facing a gap in measurements in near future Long term evolution due to CO 2 increase controlled by radiative cooling in the km heat sink Technology now exists to measure T, O, 100 to > 160 km, and to study its coupling to above and below These measurements are a priority to understanding the future of satellite operations and climate change aloft 11/20/2015 Sun-Climate Symposium
23 Beyond the Science: The Space Debris Hazard Increasing CO 2 Cooler, Less Dense Atmosphere Increases Satellite Lifetimes Increases Orbital Debris LIfteimes Do We Understand the Energy Budget of the Atmospshere above 100 km? 11/20/2015 Sun-Climate Symposium
24 Big Picture View of Space Debris NASA Orbital Debris Program Office 11/20/2015 Sun-Climate Symposium
25 Backups 11/20/2015 Sun-Climate Symposium
26 Altitude (km) 250 Existing Capability ACE Mission Capability Heat Cond. 200 CO 2, NO Cooling T NO O O-Cool CO 2, NO Cooling T O 3 CO 2 H 2 O O NO+ 50 CO 2 CO 15 11/20/2015 Sun-Climate Symposium
27 What makes the Upper Atmosphere Interesting and Worthy of Study? Blend of classical photochemistry and aeronomy Ozone is still the main radiative drive in the mesosphere and up to 90 km Solar UV variability and particle precipitation influence thermal structure and composition Climate change Expect M/LT to cool with increasing carbon dioxide Non-Equilibrium Radiative Transfer ALL heating and cooling processes occur far removed from Local Thermodynamic Equilibrium (LTE) above ~ 65 km Atomic species become significant Low density means long lifetimes for atomic oxygen and hydrogen Remarkable influence on the energy budget of the km region and above The E-region, km, is the heat sink for the entire atmosphere up to the exobase controls climate change in thermosphere/ionosphere Ultimately determines density at satellite orbits 11/20/2015 Sun-Climate Symposium
28 10 8 More Good Reasons! ~22,000 ~500,000 ~100,000,000 Marble size or larger ( 1 cm) Ball-point pen tip ( 1 mm) Softball size or larger ( 10 cm) 11/20/2015 Sun-Climate Symposium 2015 Total mass: 6,300 tonnes (2,700 tonnes in LEO) Image Courtesy Hugh Lewis U. Southampton, UK 28
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