Download ML_FoG_revisions_050509_v2 - Stanford Solar Observatories

F2B: Quantify Particle Acceleration for Key Regions of Exploration
Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction
Production and distribution of
the seed particles (pickup ions,
suprathermal plasmas in the
solar corona and planetary
magnetospheres) that are
accelerated to high energies
Required Understanding
Identify dominant processes
controlling stochastic acceleration
Quantify the dynamics of magnetic
topology and electric fields in key
regions
Quantify the critical parameters that
drive acceleration phenomena across
shock boundaries
Determine the role of parallel DC electric
field, Alfvén and low frequency waves in
acceleration process
Enabling Capabilities & Measurements
Remote and in situ particle and field
observations of the corona and nearSun acceleration regions
Models to quantify the interaction of
multiple acceleration mechanisms in
key regions
Great Observatory
Assumes launch of Solar-B, MMS, SDO,
RBSP, THEMIS, IBEX, Cluster, ITSP, L1
monitor
Enabling
LWS missions
SEPP - quantify critical parameters for the
source regions and the SEP outputs
Contributing
LWS Program
Sentinels – will observe heliospheric
acceleration shock regions created by CMEs
Contributing
STP Program
GEC– measures ionospheric control of
magnetospheric acceleration processes
Hybrid computer algorithms
focused on shock region models
in key regions
In situ and remote high temporal, spectral
and spatial resolution observations in
connected acceleration regions in nearEarth region
Spatially and temporally resolved observations of
shock interface in key regions
(Sun-Corona, SW-CME-CIR, CME-Mag, Helio-Interstellar)
Implementation Phase 2: 2015-2025
Enabling
STP Program
AAMP – mission to quantify the
acceleration processes probing the readily
available near Earth environment.
Enabling
STP Program
IMC – mission to quantify the
acceleration processes in the inner
magnetosphere
Contributing
STP Program
MTRAP - mission to explore the solar
acceleration region dominated by
magnetic pressure
Enabling
Contributing
Model/Theory Development -
What resource
SPI/Telemechus - understand solar
dynamo - put in phase 3 instead?
Flagship mission
Solar Probe – will provide obs of
acceleration process near sun
Community wide modeling workshops
focusing on model development +
Theory Program
Potential Discovery
Mission to observe in situ and quantify
interplanetary acceleration processes
at shock boundaries
Potential Explorer
Mission to observe and quantify
acceleration processes associated with
electric field in a magnetized
environment
Other Agencies
US: L1 Monitor, ATST
Foreign: ORBITALS, Ravens, Solar
Obiter
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F2C: Quantify Coupling Mechanisms at Critical Interfaces
Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction
Transfer of solar wind information through
planetary electrodynamic systems
Required Understanding
Feedback of the ionosphere on
magnetospheric electrodynamics
Meteorological Forcing of the ITM
Chemical & dynamical
coupling between upper
atmosphere disturbances & the
lower atmosphere
Detailed coupling of magnetotail
dynamics to the polar region
Controllers of mass and energy flow
between the solar wind and geospace
Transition of solar steady and eruptive events
from interior of the sun to the atmosphere
Global I-T coupling and the creation of
instabilities
Enabling Capabilities & Measurements
Simultaneous, colocated neutral
winds, ionospheric densities & drifts
Global characterization of the
current systems linking geospace
using swarms of satellites
Simultaneous multi-point
characterization of the magnetotail
and imaging of the auroral oval
Satellite observations of
atmospheric chemistry &
key dynamical features
Two-way-coupled
modeling capabilities
Multi-point measurements of solar
wind and dayside magnetopause
Simultaneous measurement of solar
reconnection features and heliospheric
density structures
Implementation Phase 2: 2015-2025
MMS, ITSP, RBSP,
SDO
The existing Great Observatory
provides necessary measurements to
understand the linkages
ITM-Waves, GEC, GEMINI,
MC, Sentinels
These are the most important missions in this
phase to address coupling mechanisms at
interfaces
Mars Dynamics
interface between the upper and lower
atmosphere at Mars
Solar Probe, SEPP, MTRAP,
DBC, AAMP, SPI/TLM
Theory/Modeling
Coupled models between
regions of space to provide
physical insight on mass
and energy transfer rates
These are missions that also could provide
critical measurements for understanding
linkages between regions
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J2A: Characterize the Near-Sun Source Region of the Space Environment
Phase 2015-2025, Safeguard the Outward Journey
Particle acceleration mechanisms
in CME shocks and CME/flare
current sheets
Relationship between CME
evolution and pre-existing solar
wind conditions
Link the solar disturbances to their
geoeffective consequences
UV Spectroscopic determination of Pre/Post-shock density,
speed, compression; ion/
electron velocity distributions,
charge states, abundances;
Alfven speed, magnetic field,
reconnection rates in CME
shocks, flares, current sheets
Required Understanding
Recognition of precursors of large
CMEs, flares and SEP events
responsible for major space weather
disturbances
Link between magnetic
field and solar wind at
all latitudes
SOLAR-B,
SDO,
SENTINELS
STP and LWS missions
from previous phases
Relationship between magnetic
flux emergence & transport
and the solar wind
Understand solar reconnection
through the planetary analog
Enabling Capabilities & Measurements
Multipoint
Visible light observations of
Coronagraph/ magnetospheric
Polarimeter for reconnection
electron density
and
evolution and reconfiguration
flow speeds
High latitude
observations of
fields &
particles
Implementation Phase 2: 2015 - 2025
Assumed Phase 1 Assets
Acceleration mechanisms and sources
of the fast and slow solar wind
Enabling
Program
LWS
SEPP to fully
characterize coronal
sources of SEPs, CME
shocks and current sheets
Contributing
Program ?
Mars Aero. Probe to
understand Solar reconnection
through the Mars analog
Enabling
Near-Sun in situ
measurements of
charged particle
distribution,
composition,
waves & fields;
neutrons, hard Xrays & gamma
rays
LWS Program
MagCon, AAMP,
GEMINI to understand Earth
analog to Solar reconn. and determine
geospace effects of Solar sources
Enabling
LWS Program
Doppler to identify
disk signatures of
CME, flare, and SEP
initiation
On-Disk UV/EUV
Spectrographic imaging for
Geospace
flow velocities, energy
observations
release signatures; Disk
to quantify
effects of Magnetograph for magnetic
solar sources field topology and evolution
Contributing
Enabling
Flagship Mission
Solar Probe for in
Partnership
Solar Orbiter for
in situ
sampling of inner heliosphere
situ sampling of inner
heliosphere
Contributing
STP Program
SPI or Telemachus
To characterize high latitude
source regions
Integrated empirical
Theory/Modeling
Program
To guide the evolution of physics
based predictive theory
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J2C: Determine Mars Atmospheric Variability Relevant to Aerocapture, Entry,
Descent, Landing, Surface, Navigation and Communications –
Phase 2015-2025, Safeguard the Outward Journey
Required Understanding
Wave-wave interactions at all
scales
Non-LTE
radiative
transfer
Dust, aerosol
evolution and
characteristics
Simultaneous and
coordinated global
measurements of
neutral & plasma
density, B-field,
temperature, winds
Neutral & plasma
instabilities
Waveturbulence
interactions
Plasma-neutral
coupling with
B-field
Lightning
To inform on tidal and tide-mean
flow processes relevant to Mars
Wave-mean flow
interactions
Enabling Capabilities & Measurements
Critical Regimes: Entry, Descent & Landing (EDL), 0-40 km; Aerocapture,
40-80 km; Aerobraking & Orbital Lifetime, 80-250 km; Ionosphere 90-200 km
Electrical & Dust
Environments
Empirical models of
global Mars atmosphere
structure & variability
Implementation Phase 1: 2005-2015
CNOFS, TIMED
Mission
Plasma
irregularities at
Earth & Mars
& effects on radio
propagation
Parameterizations of
turbulence and gravity
wave effects in GCMs
LWS Program
IT Storm Probes + ITImager Mission
To inform on plasma irregularities relevant to COMM
and NAV systems at Mars and between Earth & Mars
Mitigate ionosphere effects
on precision landing (GPS)
Implementation Phase 2: 2015-2025
Potential Scout
ITM WAVES
Theory &
Mars Dynamics
Mission
Modelling
To inform on waveMission
wave, wave-mean flow
To collect observations of
Program
processes and
What Program?
parameterizations
relevant to Mars
Theory & Modelling Program
To understand waves, instabilities, and plasma processes that determine
variabilities of Earth & Mars’ environments; develop surface to
ionopause first-principles model of Mars’ atmosphere
First principles
data-assimilating
models for
predicting global
atmosphere and
ionosphere
structure
densities, temperatures and
winds 0-100 km over all local
times at Mars
GEC
Dipper mission, Earth analog to dynamics and
variability of the lower thermosphere
To develop an
Assimilative Model for
Mars’ whole Atmosphere
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F3A: Predict Solar System Magnetic Activity and Energy Release
Targeted Outcome: 2025-beyond, Opening the Frontier
Dominant processes
controlling solar dynamo
Characterize predictability of
dynamo: analytic, statistical,
or chaotic
Required Understanding
Solar surface and interior
flows as drivers for solar
magnetic field evolution on
active region, solar cycle and
century time scales
Dominant processes controlling magnetic
structuring, energy buildup, storage, and release
Characterize predictability of magnetic energy
release
Production of paleoclimate
tracers of solar activity
Understand to the level of predictability the ionospheric dynamo
Whole-Sun remote-sensing
observations (magnetic,
velocity, XUV, EUV)
Enabling Capabilities & Measurements
Global heliosphere in-situ
observations (plasma, field,
particles)
Measurements throughout the magnetosphere of
fields and particles
Measurements throughout the ionosphere and
thermosphere of density, comp. and drifts
Active region coronal measurements of magnetic
field, velocity, thermal fine structure
Integrated solar interioratmosphere magnetic models
using observational inputs
Integrated MHD/plasma
models of coronal magnetic
heating and stability
Implementation
Enabling:
Enabling:
SHIELDS, SPI, Farside - remote sensing
MagCon: magnetotail dynamics
SWB, SPI - in-situ
IMC: inner magnetospheric dynamics
RAM, MTRAP - coronal structure
DBC: dayside magnetic structure
Enhancing:
Stellar Imager – dynamo context
Theory and Modeling:
Predictability analysis of MHD
systems
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F3B: Predict High Energy Particle Flux Throughout the Solar System
Targeted Outcome: Phase 3- 2025-beyond, Opening the Frontier
From Phase 2: Understand SW
magnetic processes and quantify
acceleration in key regions
Understand the transfer of
energetic particles between
regions of space (e.g., heliosphere
to magnetosphere)
Required Understanding
Understand the source of
dominant processes that create
energetic particles at the Sun, in
interplanetary space and within
magnetospheres
Understand transport processes of
energetic particles in interplanetary
regions in the Solar System
Understand the energization processes
across multiscalar interfaces that result in
acceleration of particles
Determine the plasma populations
throughout the Solar System
Enabling Capabilities & Measurements
Remote and in situ
particle and field
observations of key
regions where
energetic particles
are generated
Develop physics based models that predict
particle fluxes within magnetospheres
In situ observations of plasmas within
.5 AU that will
Remote and in situ observations in Geospace
and other planetary magnetospheres in order to
predict particle fluxes
Develop physics based models that
predict particle fluxes out to 1.5 AU
using solar and innerheliospheric
observations
Great Observatory
Assumes launch of ITSP, L1 monitor,
SEPP, Auroral Imagers, Solar Sentinels,
MTRAP, solar chronograph
Flagship mission
Potential Discovery
Mission to observe quantify Mercury’s
magnetospheric particle and plasma
populations
Mission to quantify the particle and
energy propagation through the solar
wind-magnetosphere-ionosphere system
IMC, MagCon, DBC, AAMP
Potential Explorer
Mission to quantify the dynamics of and
particle interaction across the
heliospheric boundary
Implementation Phase 3: 2025-beyond
Enabling
LWS missions
Solar wind mission that quantifies particle
fluxes within 1 AU and within Geospace
Contributing
LWS Program
Mission that remotely observes the solar
source of particles and impact of particles in
Geospace
Enabling
STP Program
Mission to observe the far side of the Sun
Contributing
STP Program
Mission to remotely investigate
extraterrestrial magnetospheres
Contributing
??? Program
Interstellar Probe - Measurements during
cruise phase
Enabling
Model/Theory Development Theory and Modeling program focused
on predicting particle flux and
populations throughout the Solar
System
Other Agencies
US: monitor of geoeffective solar
phenomena (chronograph?)
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F3C: Understand the Interactions of Disparate Astrophysical Systems
Targeted Outcome: Phase 3- 2025-beyond, Open the Frontier
Required Understanding
Cosmic ray interaction with
heliopause
Understand to the level of prediction
the coupling between interplanetary
medium and magnetosphereionosphere-atmosphere system
Image heliopause
Enabling Capabilities & Measurements
Image termination shock using
energetic hydrogen atoms and
radio detection
Multipoint measurements of SWmagnetosphere coupling
Heliospheric Imager &
Galactic Observer
(HIGO) To image the interaction
between interstellar medium and
heliopause
Physical structure of bow shocks
(termination shock) at heliopause,
supernova remnants, binary star
interaction regions, neutron star
spheres, and black hole horizons.
Cross-scale coupling of
galactic magnetic field between
interstellar medium and
heliosphere
The location and 3D structure of
the interaction region between the
heliosphere and local galactic
environment
Determine isotopic and elemental
composition, flow directions,
speed, and temperature of pickup
ions and neutrals with
in-situ stellar probes
In situ and remote measurements of
magnetosphere-ionosphere coupling
Measure low-energy cosmic rays
in situ with interstellar probes
Solar sail technology
to enable interstellar spacecraft
Measurements of coupling between
atmospheric layers/regions
Implementation Phase 3: 2025-2035
Interstellar Probes,
Explorers & Missions
To explore interstellar medium
Stellar Imager
To explore the magnetic activity of
other stars
Theory/Modeling
Program
To simulate shock waves in
astrophysical environments
DBC, MagCon, IMC
TITM-C, ITM-Waves, AAMP
Constellations to investigate SWmagnetospheric coupling
Missions to quantify atmospheric coupling
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