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F2B: Quantify Particle Acceleration for Key Regions of Exploration

F2B: Quantify Particle Acceleration for Key Regions of Exploration Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction. Great Observatory. Assumes launch of Solar-B, MMS, SDO, RBSP, THEMIS, IBEX, Cluster, ITSP, L1 monitor. Contributing. LWS Program.

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F2B: Quantify Particle Acceleration for Key Regions of Exploration

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  1. F2B: Quantify Particle Acceleration for Key Regions of Exploration Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction Great Observatory Assumes launch of Solar-B, MMS, SDO, RBSP, THEMIS, IBEX, Cluster, ITSP, L1 monitor Contributing LWS Program Enabling LWS missions Sentinels – will observe heliospheric acceleration shock regions created by CMEs SEPP - quantify critical parameters for the source regions and the SEP outputs Potential Discovery Other Agencies Mission to observe in situ and quantify interplanetary acceleration processes at shock boundaries US: L1 Monitor, ATST Foreign: ORBITALS, Ravens, Solar Obiter Contributing STP Program Contributing Enabling Enabling Contributing STP Program STP Program What resource STP Program Enabling MTRAP - mission to explore the solar acceleration region dominated by magnetic pressure Potential Explorer Flagship mission GEC– measuresionospheric control of magnetospheric acceleration processes IMC – mission to quantify the acceleration processes in the inner magnetosphere AAMP – mission to quantify the acceleration processes probing the readily available near Earth environment. SPI/Telemechus - understand solar dynamo - put in phase 3 instead? Mission to observe and quantify acceleration processes associated with electric field in a magnetized environment Solar Probe – will provide obs of acceleration process near sun Required Understanding Production and distribution of the seed particles (pickup ions, suprathermal plasmas in the solar corona and planetary magnetospheres) that are accelerated to high energies Quantify the critical parameters that drive acceleration phenomena across shock boundaries Identify dominant processes controlling stochastic acceleration Quantify the dynamics of magnetic topology and electric fields in key regions 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 near-Sun acceleration regions In situ and remote high temporal, spectral and spatial resolution observations in connected acceleration regions in near-Earth region Hybrid computer algorithms focused on shock region models in key regions Models to quantify the interaction of multiple acceleration mechanisms in key regions 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 Model/Theory Development - Community wide modeling workshops focusing on model development + Theory Program 1

  2. F2C: Quantify Coupling Mechanisms at Critical Interfaces Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction Required Understanding Controllers of mass and energy flow between the solar wind and geospace Transfer of solar wind information through planetary electrodynamic systems Feedback of the ionosphere on magnetospheric electrodynamics Transition of solar steady and eruptive events from interior of the sun to the atmosphere Meteorological Forcing of the ITM Chemical & dynamical coupling between upper atmosphere disturbances & the lower atmosphere Detailed coupling of magnetotail dynamics to the polar region 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 Multi-point measurements of solar wind and dayside magnetopause Satellite observations of atmospheric chemistry & key dynamical features Simultaneous measurement of solar reconnection features and heliospheric density structures Simultaneous multi-point characterization of the magnetotail and imaging of the auroral oval Two-way-coupled modeling capabilities Implementation Phase 2: 2015-2025 Theory/Modeling Coupled models between regions of space to provide physical insight on mass and energy transfer rates 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 Solar Probe, SEPP, MTRAP, DBC, AAMP, SPI/TLM These are missions that also could provide critical measurements for understanding linkages between regions Mars Dynamics interface between the upper and lower atmosphere at Mars 2

  3. 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 Required Understanding 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 magnetic flux emergence & transport and the solar wind Relationship between CME evolution and pre-existing solar wind conditions Understand solar reconnection through the planetary analog Link between magnetic field and solar wind at all latitudes Link the solar disturbances to their geoeffective consequences 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 Multipoint observations of magnetospheric reconnection and reconfiguration Near-Sun in situ measurements of charged particle distribution, composition, waves & fields; neutrons, hard X-rays & gamma rays Visible light Coronagraph/ Polarimeter for electron density evolution and flow speeds Geospace observations to quantify effects of solar sources High latitude observations of fields & particles Implementation Phase 2: 2015 - 2025 Contributing Partnership Enabling LWS Program Enabling Flagship Mission Enabling LWS Program Solar Orbiter for in situsampling of inner heliosphere MagCon, AAMP, GEMINI to understand Earth analog to Solar reconn. and determine geospace effects of Solar sources Solar Probe for in situsampling of inner heliosphere SEPP to fully characterize coronal sources of SEPs, CME shocks and current sheets Assumed Phase 1 Assets SOLAR-B, SDO, SENTINELS STP and LWS missions from previous phases Integrated empirical Theory/Modeling Program To guide the evolution of physics based predictive theory Enabling LWS Program Contributing STP Program Contributing Program ? Doppler to identify disk signatures of CME, flare, and SEP initiation SPI or Telemachus To characterize high latitude source regions Mars Aero. Probe to understand Solar reconnection through the Mars analog 3

  4. 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 Parameterizations of turbulence and gravity wave effects in GCMs Neutral & plasma instabilities Plasma irregularities at Earth & Mars & effects on radio propagation Non-LTE radiative transfer Wave-turbulence interactions Dust, aerosol evolution and characteristics Wave-mean flow interactions Plasma-neutral coupling with B-field Lightning Enabling Capabilities & Measurements First principles data-assimilating models for predicting global atmosphere and ionosphere structure Simultaneous and coordinated global measurements of neutral & plasma density, B-field, temperature, winds 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 Mitigate ionosphere effects on precision landing (GPS) Empirical models of global Mars atmosphere structure & variability Implementation Phase 1: 2005-2015 Implementation Phase 2: 2015-2025 ITM WAVES Mission To inform on wave-wave, wave-mean flow processes and parameterizations relevant to Mars What Program? Potential Scout CNOFS, TIMED Mission To inform on tidal and tide-mean flow processes relevant to Mars Theory & Modelling Program To develop an Assimilative Model for Mars’ whole Atmosphere Mars Dynamics Mission To collect observations of densities, temperatures and winds 0-100 km over all local times at Mars LWS Program IT Storm Probes + ITImager Mission To inform on plasma irregularities relevant to COMM and NAV systems at Mars and between Earth & 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 GEC Dipper mission, Earth analog to dynamics and variability of the lower thermosphere 4

  5. F3A: Predict Solar System Magnetic Activity and Energy Release Targeted Outcome: 2025-beyond, Opening the Frontier Dominant processes controlling solar dynamo 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 dynamo: analytic, statistical, or chaotic Characterize predictability of magnetic energy release Production of paleoclimate tracers of solar activity Understand to the level of predictability the ionospheric dynamo Enabling Capabilities & Measurements Whole-Sun remote-sensing observations (magnetic, velocity, XUV, EUV) Integrated solar interior-atmosphere magnetic models using observational inputs Active region coronal measurements of magnetic field, velocity, thermal fine structure Global heliosphere in-situ observations (plasma, field, particles) Measurements throughout the magnetosphere of fields and particles Integrated MHD/plasma models of coronal magnetic heating and stability Measurements throughout the ionosphere and thermosphere of density, comp. and drifts Implementation Enabling: Enhancing: Enabling: SHIELDS, SPI, Farside - remote sensing MagCon: magnetotail dynamics Stellar Imager – dynamo context IMC: inner magnetospheric dynamics SWB, SPI - in-situ Theory and Modeling: Predictability analysis of MHD systems RAM, MTRAP - coronal structure DBC: dayside magnetic structure 5

  6. F3B: Predict High Energy Particle Flux Throughout the Solar System Targeted Outcome: Phase 3- 2025-beyond, Opening the Frontier Great Observatory Assumes launch of ITSP, L1 monitor, SEPP, Auroral Imagers, Solar Sentinels, MTRAP, solar chronograph Contributing LWS Program Enabling LWS missions Mission that remotely observes the solar source of particles and impact of particles in Geospace Solar wind mission that quantifies particle fluxes within 1 AU and within Geospace Potential Discovery Other Agencies Mission to observe quantify Mercury’s magnetospheric particle and plasma populations US: monitor of geoeffective solar phenomena (chronograph?) Contributing Contributing ??? Program STP Program Mission to remotely investigate extraterrestrial magnetospheres Interstellar Probe - Measurements during cruise phase Enabling STP Program Enabling Potential Explorer Flagship mission Mission to observe the far side of the Sun Mission to quantify the dynamics of and particle interaction across the heliospheric boundary Mission to quantify the particle and energy propagation through the solar wind-magnetosphere-ionosphere system IMC, MagCon, DBC, AAMP From Phase 2: Understand SW magnetic processes and quantify acceleration in key regions Required Understanding Understand transport processes of energetic particles in interplanetary regions in the Solar System Understand the source of dominant processes that create energetic particles at the Sun, in interplanetary space and within magnetospheres Understand the transfer of energetic particles between regions of space (e.g., heliosphere to magnetosphere) 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 In situ observations of plasmas within .5 AU that will Develop physics based models that predict particle fluxes within magnetospheres Develop physics based models that predict particle fluxes out to 1.5 AU using solar and innerheliospheric observations Remote and in situ observations in Geospace and other planetary magnetospheres in order to predict particle fluxes Implementation Phase 3: 2025-beyond Model/Theory Development - Theory and Modeling program focused on predicting particle flux and populations throughout the Solar System 6

  7. F3C: Understand the Interactions of Disparate Astrophysical Systems Targeted Outcome: Phase 3- 2025-beyond, Open the Frontier Required Understanding Cosmic ray interaction with heliopause Cross-scale coupling of galactic magnetic field between interstellar medium and heliosphere Physical structure of bow shocks (termination shock) at heliopause, supernova remnants, binary star interaction regions, neutron star spheres, and black hole horizons. Understand to the level of prediction the coupling between interplanetary medium and magnetosphere-ionosphere-atmosphere system The location and 3D structure of the interaction region between the heliosphere and local galactic environment Enabling Capabilities & Measurements Image heliopause Measure low-energy cosmic rays in situ with interstellar probes Determine isotopic and elemental composition, flow directions, speed, and temperature of pickup ions and neutrals with in-situ stellar probes Image termination shock using energetic hydrogen atoms and radio detection Solar sail technology to enable interstellar spacecraft Multipoint measurements of SW-magnetosphere coupling In situ and remote measurements of magnetosphere-ionosphere coupling Measurements of coupling between atmospheric layers/regions Implementation Phase 3: 2025-2035 Heliospheric Imager & Galactic Observer (HIGO) To image the interaction between interstellar medium and heliopause Theory/Modeling Program To simulate shock waves in astrophysical environments Interstellar Probes, Explorers & Missions To explore interstellar medium Stellar Imager To explore the magnetic activity of other stars DBC, MagCon, IMC Constellations to investigate SW-magnetospheric coupling TITM-C, ITM-Waves, AAMP Missions to quantify atmospheric coupling 7

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