F1B: Determine the Dominant Processes of Particle Acceleration

1
F1B Determine the Dominant Processes of Particle
Acceleration Phase 2005-2015, Open the Frontier
Required Understanding
Shock acceleration processes
Role of seed particle population
Role of magnetic field topology
Coherent electric field acceleration

• Primary acceleration sites
• - Coronal Mass Ejection Shocks
• Solar flares, Current Sheets
• - Bow shocks, Radiation Belts
• Magnetotails, Auroral Zones
• Termination Shock

Output Energy Spectrum and Composition
Stochastic acceleration processes
Thermal plasma (solar wind) acceleration
Waves, turbulence intermittent processes
Enabling Capabilities Measurements
UV Spectroscopic determin- ation 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
Multi-point in-situ determinations of mag-
netospheric energetic particles fields at
micro/meso-scales
Multi-point In-situ measurements of density,
temperature, velocity, energy spectrum, and
charge state of particles and electric/magnetic
fields at coronal heliospheric shocks
Near-Sun measurements of neutrons, hard X-rays
gamma rays
Neutral Energetic Ion Imaging of Termination Shock
Visible light Coronagraph/ Polarimeter for
electron density evolution and flow speeds
Implementation Phase 1 2005-2015
Existing Assets
STP Program
Enabling
LWS Program
Contributing
LWS Program
Enabling
ACE, SOHO, Wind, RHESSI, Cluster, IMAGE, Polar,
FAST, TIMED, Voyager Current missions for
particle acceleration
Integrated Empirical Theory/Modeling Program To
guide the evolution of physics based predictive
theory
STEREO, Solar-B For acceleration at CME/flare
sites
RBSP In-situ observation of acceleration
processes, geospace sources of energetic
particles Inner Heliospheric Sentinels Characteriz
e SEP coronal source regions and emissions
SDO For acceleration at CME/flare
sites IT-Imager Role of ionospheric conductivity
for auroral acceleration
Explorer Program
Contributing
Potential Explorer
Enabling
THEMIS, IBEX Explorer Missions for particle
acceleration at I/F
NESCE Near-Earth Solar Coronal Explorer
Characterize SEP coronal source regions
emissions
2
H2A Identify Precursors of Important Solar
Disturbances Targeted Outcome Phase 2-
2015-2025, Opening the Frontier
Targeted Understanding
CME magnetic field orientation
Buildup of energy helicity in coronal magnetic
fields
Relationship between eruptive filaments, active
regions, CMEs, and SEPs
Relationship between CME shocks, flare/ CME
current sheets and Solar Energetic Particles
(SEPs)
Evolution of global solar magnetic field
Relationship between global field and solar
disturbances
Enabling Capabilities Measurements
Coronal vector magnetic field evolution and
subsurface field evolution
Radio burst measurements of near-Sun CME shocks
CME magnetic field evolution behind the disk
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
On-Disk UV/EUV Spectrographic imaging for flow
velocities, energy release signatures Disk
Magnetograph for magnetic field topology and
evolution
Near-Sun in situ measurements of charged particle
distribution, comp-osition, waves fields
neutrons, hard X-rays gamma rays
Visible light Coronagraph/ Polarimeter for
electron density structure and evolution
Implementation Phase 2 2015-2025
Contributing LWS Program
SHIELDS for tracking disk features behind the limb
Enabling LWS Program
Enabling STP Program
SEPP to fully characterize coronal sources of
SEPs, CME shocks and current sheets DOPPLER to
identify disk signatures of CME, flare, SEP
initiation
Existing Assets
RAM to identify disk signatures of CME, flare,
SEP initiation
Enabling Flagship Mission
SDO for global magnetic field and active region
measurements
Solar Probe for near-Sun in situ observations
Contributing STP Program
SIRA to characterize CME shocks
Contributing Partnership
Solar Orbiter for near-Sun in situ observations
3
Required Understanding
Particle acceleration mechanisms in CME shocks
and CME/flare current sheets
Acceleration mechanisms and sources of the fast
and slow solar wind
Recognition of precursors of large CMEs, flares
and SEP events responsible for major space
weather disturbances
Relationship between CME evolution and
pre-existing solar wind conditions
Relationship between magnetic flux emergence
transport and the solar wind
Link between magnetic field and solar wind at all
latitudes
Enabling Capabilities Measurements
UV Spectroscopic determin- ation 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
On-Disk UV/EUV Spectrographic imaging for flow
velocities, energy release signatures Disk
Magnetograph for magnetic field topology and
evolution
Visible light Coronagraph/ Polarimeter for
electron density evolution and flow speeds
Near-Sun in situ measurements of charged particle
distribution, composition, waves fields
neutrons, hard X-rays gamma rays
High latitude observations of fields particles
Implementation Phase 2 2015 - 2025
Contributing Partnership
Enabling Flagship Mission
Solar Orbiter for in situ sampling of inner
heliosphere
Solar Probe for in situ sampling of inner
heliosphere
Assumed Phase 1 Assets
STEREO, SOLAR-B, SDO, SENTINELS STP and LWS
missions from previous phases
Enabling LWS Program
Enabling LWS Program
SEPP to fully characterize coronal sources of
SEPs, CME shocks and current sheets
Doppler to identify disk signatures of CME,
flare, and SEP initiation
Integrated empirical Theory/Modeling Program To
guide the evolution of physics based predictive
theory
Contributing STP Program
SPI or Telemachus To characterize high latitude
source regions