Special Sensor Ultraviolet Spectrographic Imager on DMSP and Beyond Dr Larry J Paxton SSUSI Principal Investigator and Head of Geospace and Earth Science Group Bob Schaefer John Hicks Yongliang ID: 396312
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SSUSI and SSUSI-LiteSpecial Sensor Ultraviolet Spectrographic Imager on DMSP and Beyond
Dr. Larry J. PaxtonSSUSI Principal Investigator and Head of Geospace and Earth Science GroupBob Schaefer, John Hicks, Yongliang Zhang, Ethan Miller, Bernie Ogorzalek, Brian Wolven, Guiseppe Romeo and the SSUSI Team
SEASONS ConferenceSlide2
What is Space Weather?Slide3
Solar radiation Chain
Solar Wind/Magnetospheric Chain
Solar Energetic Particle Chain
Lower Atmospheric ChainSlide4
What is Space Weather?Slide5
What is Space Weather?
Space weather is the departure of the space environment from the average or climatological mean.There may be seasonal or longer term variations in the average conditions (e.g. solar cycle or seasonal effects).These variations have impacts on human systems.Establishing global climatology and the variations about those mean conditions enables us to design a cost-effective, robust system.
We must combine “good enough” scientific understanding with appropriate technology to produce a useful solution.Slide6
Nearly all C4ISR activities involving RF and space assets (or targets) are susceptible to ionospheric space weather effects to varying degrees.Many effects consitute
small risk factors, analogous to wind impacts on aircraft fuel burn, that may impact mission success. However, even apparently minor irregularities of the ionosphere may have severe impact on casualties, order of battle, and OUTCOMES: e.g., Takur-Ghar.Ionospheric effectsRefraction (bending) introduces position error in Doppler or single-site location, over-the-horizon radar techniques. Delays introduce ranging errors.Irregularities blind or dazzle radars with clutter, scramble nav/com signals (“scintillations”)
.
Ionosphere Impacts on C4ISR
Regions of scintillation, radar clutterSlide7
Space Capability Joint Effect
Environmental Cause
Environmental Effects
Potential Warfighter Impacts
Precision Engagement
Ionospheric scintillation, ionospheric refraction
Degraded GPS (or alternative navigation) system performance
GPS guided weapons miss target, increased collateral damage/civilian casualties
Intelligence
Aurora, upper atmospheric density change, ionospheric refraction and scintillation
Decreased intelligence system performance
Inaccurate enemy position data
Spacecraft anomaly assessment
Solar/Magnetospheric particle radiation,
Upper atmospheric density change, ionospheric refraction and scintillation
Satellite system anomalies, increased operational downtime of space system
Decreased operational space system utility (GPS, Space-Base Infra-Red System (SBIRS), Space Radar (SR), etc.)
Attack Assessment
Solar/Magnetosphere particle radiation,
auroral, upper atmospheric and ionospheric changes
Enemy and friendly weapon system performance degradation
Inability to meet attack assessment timelines, inability to distinguish hostile attack from natural effects
SSUSI Environmental Data Records shown in RED
SSUSI
can Help
Operators Distinguish Environmental from Deliberate EffectsSlide8
SSUSI can Help Operators Distinguish Environmental from Deliberate Effects
Space Capability Joint Effect
Environmental Cause
Environmental Effects
Potential Warfighter Impacts
Comms
on the Move
Ionospheric scintillation, ionospheric refraction
Degraded/broken communication link, anomalous radio wave propagation
Loss of command and control, lives/missions at risk
Space
situational
awareness
Upper atmospheric density change, ionospheric refraction and scintillation
Inaccurate space object identification and tracking
Space object collision (e.g. shuttle), inaccurate enemy space force position
Missile Warhead Detection/ Tracking/ Intercept
Aurora, upper atmospheric density change, ionospheric refraction and scintillation
, clouds, atmospheric attenuation
Degraded warhead detection and tracking
Decreased probability of missile intercept, lives at risk
SSUSI Environmental Data Records shown in REDSlide9
SSUSI Heritage and Relationship to Other ProgramsSlide10
SSUSI Heritage and Relationship to Other ProgramsSlide11
FUV Spectral Region Exhibits the Signatures of Space Weather
HI (121.6 nm)
OI (130.4 nm)
OI (135.6 nm)
N
2
(LBHs)
N
2
(LBHl)
Dayside Limb
H profiles and escape rate
1
Amount of O
2
absorption
1
O altitude profile
Amount of O
2
as seen in absorption
N
2
, Temperature
Dayside Disk
Column HAmount of O2 absorption1 Used with LBHs to form O/N2N2, Solar EUVSolar EUVNightside Limb
H profile and escape rateIon/ENA precipitation
EDP
HmF2
NmF2
T
plasma
Ion/ENA precipitation characteristic energy
Ion/ENA precipitation characteristic energy
Nightside Disk
Geocorna and
Ion/ENA precipitation
Ion/ENA precipitation
ò
n
e
2
ds (line of sight) and
ò
n
e
dz (vertical TEC)
Ion/ENA precipitation
Ion/ENA precipitation
Ion/ENA precipitation
Auroral
Zone
Region of proton precipitation
Auroral Boundary and amount of column O
2
present
1
Region of electron and (possibly) proton precipitation
Used with
LBHl
to form
Eo
and the ionization rate and conductance
information
Hemispheric power
Radar clutter
Charging
Measure of the effective precipitating flux, used with
LBHl
to form
Eo
and the ionization rate and conductance informationSlide12
FUV Spectral Region Exhibits the Signatures of Space Weather
HI (121.6 nm)
OI (130.4 nm)
OI (135.6 nm)
N
2
(LBHs)
N
2
(LBHl)
Dayside Limb
H profiles and escape rate
1
Amount of O
2
absorption
1
O altitude profile
Amount of O
2
as seen in absorption
N
2
, Temperature
Dayside Disk
Column HAmount of O2 absorption1 Used with LBHs to form O/N2N2, Solar EUVSolar EUVNightside Limb
H profile and escape rateIon/ENA precipitation
EDP
HmF2
NmF2
T
plasma
Ion/ENA precipitation characteristic energy
Ion/ENA precipitation characteristic energy
Nightside Disk
Geocorna and
Ion/ENA precipitation
Ion/ENA precipitation
ò
ne2ds (line of sight) and ònedz (vertical TEC)Ion/ENA precipitationIon/ENA precipitationIon/ENA precipitationAuroral ZoneRegion of proton precipitationAuroral Boundary and amount of column O2 present1Region of electron and (possibly) proton precipitationUsed with LBHl to form Eo and the ionization rate and conductance informationHemispheric powerRadar clutterChargingMeasure of the effective precipitating flux, used with LBHl to form Eo and the ionization rate and conductance informationSlide13
FUV Spectral Region Exhibits the Signatures of Space Weather
HI (121.6 nm)
OI (130.4 nm)
OI (135.6 nm)
N
2
(LBHs)
N
2
(LBHl)
Dayside Limb
H profiles and escape rate
1
Amount of O
2
absorption
1
O altitude profile
Amount of O
2
as seen in absorption
N
2
, Temperature
Dayside Disk
Column HAmount of O2 absorption1 Used with LBHs to form O/N2N2, Solar EUVSolar EUVNightside Limb
H profile and escape rateIon/ENA precipitation
EDP
HmF2
NmF2
T
plasma
Ion/ENA precipitation characteristic energy
Ion/ENA precipitation characteristic energy
Nightside Disk
Geocorna and
Ion/ENA precipitation
Ion/ENA precipitation
ò
ne2ds (line of sight) and ònedz (vertical TEC)Ion/ENA precipitationIon/ENA precipitationIon/ENA precipitationAuroral ZoneRegion of proton precipitationAuroral Boundary and amount of column O2 present1Region of electron and (possibly) proton precipitationUsed with LBHl to form Eo and the ionization rate and conductance informationHemispheric powerRadar clutterChargingMeasure of the effective precipitating flux, used with LBHl to form Eo and the ionization rate and conductance informationSlide14
APL Combines Heritage, Science, Engineering and Dual-Use TechnologyIn 1990, SSUSI started out as an
experiment on DMSP Block 5D3 (F16-F20). After development of the space weather mission, SSUSI is on the path to operational use.SSUSI/SSUSI-Lite team understands scientific principles and operational effects.Over time, the sensor role changed from an instrument that took auroral images to a scientific instrument capable of providing
Auroral
images
Auroral
energy inputs
Auroral ionospheric productsIonospheric imagesIonospheric bubble mapsNeutral atmosphere compositionHigh energy particle precip
. mapsMagnetic field maps for s/c chargingInputs to operational modelsWe continue to develop new productsMust go beyond “science” to products that directly support decisions and planning.Slide15
SSUSI has a Unique Ability: 3D Imaging of the IonosphereSSUSI scan pattern enables us to recover a 3D image of the ionosphere from the horizon-to-horizon + limb scan information.
About 100,000 line of sight TEC measurement per da per SSUSISlide16
SSUSI has a Unique Ability: 3D Imaging of the IonosphereSSUSI scan pattern enables us to recover a 3D image of the ionosphere from the horizon-to-horizon + limb scan information.Slide17
SSUSI has a Unique Ability: 3D Imaging of the IonosphereSSUSI scan pattern enables us to recover a 3D image of the ionosphere from the horizon-to-horizon + limb scan information.Slide18
F19 Allows Us to Trace the Evolution of Ionospheric Bubbles“Space bubble” forming earlier in the evening (observed by F19 evolves and drifts and is seen later by F18)
F19 SSUSI 6:30 pm
F18 SSUSI
8
:
0
0 pm
Bubble grows and drifts
Predictive capabilitySlide19
SSUSI-Lite: Smaller, More-Capable SSUSISSUSI-Lite demonstrated that we could be build a new, better version of SSUSI.
Focused on the electronicsTRL 6 demonstration of electronics and scan mechanismGreater flexibility and on-board processing½ the mass and ½ the power – greater capabilityUses heritage algorithms to produce products for warfighter – high reuse of codeA new version could be even lighter and smaller
SSUSI conceptual design is solid and still meets requirements
Technologies have changed.Slide20
SSUSI Images the InvisibleThe full potential of operational SSUSI is not yet available to users.
SSUSI and SSUSI-Lite provide a fine-scale view of the ionosphereAPL has developed models that can exploit the native SSUSI/SSUSI-Lite resolution.Flexible scan pattern with SSUSI-Lite can be optimized on-the-fly for theater-level products w/realtime downlink and processing at the local siteSlide21
GPS-RO and SSUSI/SSUSI-Lite: A Powerful Combination
GPS total electron content (TEC) and radio occultation (RO) are other sensors widely used to drive operational models.Strengths are low unit cost, synergy with other activities (geodesy, tectonics, meteorology)Weaknesses are coverage (and total cost to achieve coverage), inability to locate scintillation-causing regions unambiguously; provides little information about aurora.
SSUSI-Lite plus GPS occultation is a powerful combination
. Slide22
Ice-Free Arctic Will Become a Theater of Interest
From DoD Arctic Strategy –November 2013: “This strategy identifies the Department’s desired end-state for the Arctic: a secure and stable region where U.S. national interests are safeguarded, the U.S. homeland is protected, and nations work cooperatively to address challenges. It also articulates two main supporting objectives:
Ensure security, support safety, and promote defense cooperation, and prepare to respond to a wide range of challenges and contingencies
—”Slide23
SSUSI Maps the Polar RegionSSUSIs combine to map the polar region
F19 adds information about polar aurora extent and evolution11/16/2014 – 0100 UT
F18
F19Slide24
SSUSI is the Only Sensor Providing Global Scale
Auroral ImageryRadar, comm, and navigation are affected by aurora overhead or along the propagation path
Region of potential radar clutter.Slide25
SSUSI: Past, Present and FutureThe SSUSI program embodies many of the best qualities of APLLong term commitment to a program of
national importanceHighest quality possible commensurate with a cost-effective approachCommitment to deliver products to the user communityCommitment to connecting research and applications communities
The next SSUSI is slated for launch on DMSP F20
Currently slated for late 2016
F20 satellite is ready to go but was the first built
SSUSI-Lite is the next step in the evolution of the APL sensor line
Half the mass, power and volume with more capability
Supports next-gen algorithms and beyondBuilds on 75,000 lines of operational code already running operationallyFlexible design can be accommodated on a variety of platforms including small satellites and hosted payloadsCould provide information in real-time for tailored local products.Slide26Slide27
Ionospheric profiles(Day and Night)Scintillation mapsAuroral characterizationLEO Energetic Particles
Neutral Density ProfilesTemperaturesNeeds Identified in JROCM 091-12
Cat A measurements
Cat B measurementsSlide28
What is Space Weather?