Transcript SSUSI-Lite

SSUSI and SSUSI-Lite
Special Sensor Ultraviolet Spectrographic Imager
on DMSP and Beyond
SEASONS Conference
Dr. Larry J. Paxton
SSUSI Principal Investigator and
Head of Geospace and Earth Science Group
Bob Schaefer, John Hicks, Yongliang Zhang,
Ethan Miller, Bernie Ogorzalek, Brian
Wolven, Guiseppe Romeo and the SSUSI
Team
What is Space Weather?
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Solar Energetic Particle Chain
Solar radiation Chain
Solar Wind/Magnetospheric Chain
Lower Atmospheric Chain
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What is Space Weather?
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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.
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Ionosphere Impacts on C4ISR
 Nearly all C4ISR activities involving
RF and space assets (or targets) are
susceptible to ionospheric space
weather effects to varying degrees.
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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 effects
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Refraction (bending) introduces
position error in Doppler or singlesite location, over-the-horizon radar
techniques.
Delays introduce ranging errors.
Irregularities blind or dazzle radars
with clutter, scramble nav/com
signals (“scintillations”).
Regions of scintillation, radar clutter
SSUSI can Help Operators Distinguish Environmental
from Deliberate Effects
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
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SSUSI can Help Operators Distinguish Environmental from
Deliberate Effects
Space Capability
Joint Effect
Comms on the
Move
Environmental Cause
Ionospheric scintillation,
ionospheric refraction
Environmental
Effects
Degraded/broken
communication
link, anomalous
radio wave
propagation
Inaccurate space
object identification
and tracking
Space situational
awareness
Upper atmospheric
density change,
ionospheric refraction
and scintillation
Missile Warhead
Detection/
Tracking/
Intercept
Aurora, upper atmospheric Degraded warhead
density change,
detection and
tracking
ionospheric refraction
and scintillation, clouds,
atmospheric attenuation
SSUSI Environmental Data Records shown in RED
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Potential Warfighter
Impacts
Loss of command and
control,
lives/missions at
risk
Space object collision
(e.g. shuttle),
inaccurate enemy
space force
position
Decreased probability
of missile intercept,
lives at risk
SSUSI Heritage and Relationship to Other Programs
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SSUSI Heritage and Relationship to Other Programs
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FUV Spectral Region Exhibits the Signatures of
Space Weather
HI (121.6 nm)
OI (130.4 nm)
OI (135.6 nm)
N2 (LBHs)
N2 (LBHl)
Dayside
Limb
H profiles and
escape rate1
Amount of O2
absorption1
O altitude profile
Amount of O2 as
seen in
absorption
N2, Temperature
Dayside
Disk
Column H
Amount of O2
absorption1
Used with LBHs
to form O/N2
N2, Solar EUV
Solar EUV
Nightside
Limb
H profile and
escape rate
Ion/ENA
precipitation
EDP
HmF2
NmF2
Tplasma
Ion/ENA
precipitation
characteristic
energy
Ion/ENA
precipitation
characteristic
energy
Nightside
Disk
Geocorna and
Ion/ENA
precipitation
Ion/ENA
precipitation
ne2ds (line of
sight) and
nedz (vertical
TEC)
Ion/ENA
precipitation
Ion/ENA
precipitation
Ion/ENA
precipitation
Auroral
Zone
Region of proton
precipitation
Auroral Boundary
and amount of
column O2
present1
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
information
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FUV Spectral Region Exhibits the Signatures of
Space Weather
HI (121.6 nm)
OI (130.4 nm)
OI (135.6 nm)
N2 (LBHs)
N2 (LBHl)
Dayside
Limb
H profiles and
escape rate1
Amount of O2
absorption1
O altitude profile
Amount of O2 as
seen in
absorption
N2, Temperature
Dayside
Disk
Column H
Amount of O2
absorption1
Used with LBHs
to form O/N2
N2, Solar EUV
Solar EUV
Nightside
Limb
H profile and
escape rate
Ion/ENA
precipitation
EDP
HmF2
NmF2
Tplasma
Ion/ENA
precipitation
characteristic
energy
Ion/ENA
precipitation
characteristic
energy
Nightside
Disk
Geocorna and
Ion/ENA
precipitation
Ion/ENA
precipitation
ne2ds (line of
sight) and
nedz (vertical
TEC)
Ion/ENA
precipitation
Ion/ENA
precipitation
Ion/ENA
precipitation
Auroral
Zone
Region of proton
precipitation
Auroral Boundary
and amount of
column O2
present1
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
information
12
FUV Spectral Region Exhibits the Signatures of
Space Weather
HI (121.6 nm)
OI (130.4 nm)
OI (135.6 nm)
N2 (LBHs)
N2 (LBHl)
Dayside
Limb
H profiles and
escape rate1
Amount of O2
absorption1
O altitude profile
Amount of O2 as
seen in
absorption
N2, Temperature
Dayside
Disk
Column H
Amount of O2
absorption1
Used with LBHs
to form O/N2
N2, Solar EUV
Solar EUV
Nightside
Limb
H profile and
escape rate
Ion/ENA
precipitation
EDP
HmF2
NmF2
Tplasma
Ion/ENA
precipitation
characteristic
energy
Ion/ENA
precipitation
characteristic
energy
Nightside
Disk
Geocorna and
Ion/ENA
precipitation
Ion/ENA
precipitation
ne2ds (line of
sight) and
nedz (vertical
TEC)
Ion/ENA
precipitation
Ion/ENA
precipitation
Ion/ENA
precipitation
Auroral
Zone
Region of proton
precipitation
Auroral Boundary
and amount of
column O2
present1
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
information
13
APL Combines Heritage, Science, Engineering and
Dual-Use Technology
 In 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
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Auroral images
Auroral energy inputs
Auroral ionospheric products
Ionospheric images
Ionospheric bubble maps
Neutral atmosphere composition
High energy particle precip. maps
Magnetic field maps for s/c charging
Inputs to operational models
 We continue to develop new products
 Must go beyond “science” to products that directly support
decisions and planning.
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SSUSI has a Unique Ability: 3D Imaging of the
Ionosphere
 SSUSI 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 SSUSI
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SSUSI has a Unique Ability: 3D Imaging of the
Ionosphere
 SSUSI scan pattern enables us to recover a 3D image of the
ionosphere from the horizon-to-horizon + limb scan information.
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SSUSI has a Unique Ability: 3D Imaging of the
Ionosphere
 SSUSI scan pattern enables us to recover a 3D image of the
ionosphere from the horizon-to-horizon + limb scan information.
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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
Bubble grows and drifts
Predictive capability
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F18 SSUSI 8:00 pm
SSUSI-Lite: Smaller, More-Capable SSUSI
• SSUSI conceptual design is solid and still meets requirements
• Technologies have changed.
 SSUSI-Lite demonstrated that we
could be build a new, better version
of SSUSI.
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Focused on the electronics
TRL 6 demonstration of electronics
and scan mechanism
Greater flexibility and on-board
processing
½ the mass and ½ the power –
greater capability
Uses heritage algorithms to produce
products for warfighter – high reuse
of code
 A new version could be even lighter
and smaller
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SSUSI Images the Invisible
 The full potential of operational SSUSI is
not yet available to users.
 SSUSI and SSUSI-Lite provide a fine-scale
view of the ionosphere
 APL 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 site
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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.
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Ice-Free Arctic Will Become a Theater of Interest
From DoD Arctic Strategy –November 2013: “This
strategy identifies the Department’s desired endstate 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—”
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SSUSI Maps the Polar Region
 SSUSIs combine
to map the polar
region
 F19 adds
information
about polar
aurora extent
and evolution
 11/16/2014 –
0100 UT
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F19
F18
SSUSI is the Only Sensor Providing Global Scale
Auroral Imagery
Region of
potential
radar clutter.
Radar, comm, and
navigation are
affected by aurora
overhead or along
the propagation
path
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SSUSI: Past, Present and Future
 The SSUSI program embodies many of the best qualities of APL
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Long term commitment to a program of national importance
Highest quality possible commensurate with a cost-effective approach
Commitment to deliver products to the user community
Commitment to connecting research and applications communities
 The next SSUSI is slated for launch on DMSP F20
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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
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Half the mass, power and volume with more capability
Supports next-gen algorithms and beyond
– Builds on 75,000 lines of operational code already running operationally
Flexible design can be accommodated on a variety of platforms including
small satellites and hosted payloads
Could provide information in real-time for tailored local products.
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Needs Identified in JROCM 091-12
Cat A
measurements
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Ionospheric profiles(Day and Night)
Scintillation maps
Auroral characterization
LEO Energetic Particles
Cat B
measurements
 Neutral Density Profiles
 Temperatures
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What is Space Weather?
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