Targeted Outcome: Phase 2005-2015, Opening the Frontier

1. F1A: Targeted Outcome to Capabilities to Implementation Targeted Outcome: Phase 2005-2015, Opening the Frontier Characterize magnetic reconnection at the Sun and the Earth Required Understanding What mechanisms lead to onset of reconnection? What instabilities lead to global effects? To elucidate the role of microphysics, meso-scales, global topology and cross-scale coupling in reconnection What are the mechanisms and regions of particle acceleration within the reconnection geometry? Where are the reconnection regions and what is their topology? Observations of solar wind conditions near 1 AU to provide information on drivers of geospace reconnection Enabling Capabilities & Measurements New simulation techniques to incorporate microphysics into large-scale systems to enable modeling of complete reconnection process, including cross-scale coupling and large scale topology In situ electron and ion temporal-scale particle distributions, and 3d fields from quasi-static to electron plasma frequency within reconnection regions on satellite clusters with variable spacing from few km to 100s km High resolution imaging multiple wavelengths to measure dynamics of magnetic fields from photosphere through corona Complementary missions to study precursors or results of reconnection Implementation Phase 1: 2005-2015 THEMIS -substorm dynamics Solar B -solar magnetic fields STEREO-CMEs RBSP-particle acceleration SDO -solar magnetic variability and large scale, structure RHESSI- Other Agencies Theory/Modeling To apply insights obtained from in situ observations of geospace reconnection to large scale simulations to enable predictive capabilities at the Sun and Earth Enabling STP mission Explorer Candidates L1 Monitor - to provide solar wind conditions Auroral Imaging - to monitor substorm onsets and energy dissipation MMS To fully resolve microphysics and cross-scale coupling processes of reconnection using in-situ at the Earth’s magnetosphere relevant to reconnection throughout cosmos Solar mission – To determine/study small-scale signatures of magnetic reconnection at the Sun

2. F1B: Determine the Dominant Processes of Particle Acceleration Phase 2005-2015, Open the Frontier Required Understanding Shock acceleration processes Role of seed particle population Coherent electric field acceleration Role of magnetic field topology • Primary acceleration sites: • - Coronal Mass Ejection Shocks • Solar flares, Current Sheets • - Bow shocks, Radiation Belts • Magnetotails, Auroral Zones • Termination Shock Thermal plasma (solar wind) acceleration Stochastic acceleration processes Output Energy Spectrum and Composition 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 Near-Sun measurements of neutrons, hard X-rays & gamma rays Multi-point In-situ measurements of density, temperature, velocity, energy spectrum, and charge state of particles; and electric/magnetic fields at coronal & heliospheric shocks 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 Enabling STP Program Contributing LWS Program Enabling LWS Program ACE, SOHO, Wind, RHESSI, Cluster, IMAGE, Polar, FAST, TIMED, Voyager Current missions for particle acceleration MMS- acceleration in reconnection STEREO, Solar-B For acceleration at CME/flare sites SDO For acceleration at CME/flare sites IT-Imager; GEC Role of ionospheric conductivity for auroral acceleration RBSP In-situ observation of acceleration processes, geospace sources of energetic particles Sentinels to characterize acceleration, injection and transport of SEPs Solar Probe In-situ observation of acceleration Integrated Empirical Theory/Modeling Program To guide the evolution of physics based predictive theory Contributing Explorer Program Enabling Potential Explorer NESCE [Near-Earth Solar Coronal Explorer] Characterize SEP coronal source regions & emissions THEMIS, IBEXExplorer Missions for particle acceleration at I/F High alt rocket-lower alt auroral acceleration 2

3. F1C:Identify key processes that couple regions from solar and planetary atmospheres to the heliosphere and beyond Required Understanding To elucidate cross-scale coupling in all regions from the Sun through the Earth’s atmosphere and into interplanetary space Evolution of emerged solar magnetic flux under coupled interaction between differential rotation and small-scale fluid and plasma transport mechanisms Role of shocks, wave-wave and wave-particle interactions in coupling Transition from magnetically dominated to flow dominated processes Change of scale sizes across boundaries Generation, transport, and evolution of solar open flux regions Role of turbulence in coupling to very large scales Important scale sizes for coupling in the solar atmosphere and the solar wind? Enabling Capabilities & Measurements Current and near future in-situ, and remote measurements and imaging from SEC Great Observatory New simulation techniques to incorporate turbulence on a microscale into large-scale systems Multi-view remote-sensing solar observations (white light, XUV, radio-wave), multi-point in-situ solar wind observations (plasma, field, particles) to the heliosphere and beyond Multi-spacecraft & cluster ionospheric/ magnetospheric in situ measurements and imaging combined with solar EUV and soft x-ray input High time resolution imaging of multiple layers in the solar atmosphere coronal magnetic field measurements & helioseismology Wind and wave interactions in the ionosphere and mesosphere Deep-space observations of heliospheric boundary Implementation Phase 1: 2005-2015 Enabling STP Program Existing Assets Theory/Modeling Program To enable solar, heliospheric and geospace modeling to understand couplings Cluster, STEREO, TIMED, L1/ Earth multi-measurementsTo elucidate solar wind cross-scale coupling and the change of scale sizes across boundaries. TIMED for elucidate winds, waves, and resulting interaction across temporal and spatial scales. Prototyping: ACE, SOHO, STEREO, WIND, SDO, Solar B Great Observatory MMS To observe scale lengths of reconnection in situ and determine the importance of microturbulence Enabling LWS Program SDO, IT Storm Probes + ITImager To determine the important scale size coupling in the solar atmosphere and to provide input for ionospheric ITImager is for thermospheric tidal structure. SDO for helioseismology and solar imaging Enabling Explorer Program IBEXI to image heliospheric boundaries; ISP to characterize boundary regions of solar wind- interstellar medium interaction SPI/Telemachus to observe solar wind structure and high latitudes SWB to observe solar wind structure at all longitudes Enabling STP GEC - Observe energy/momentum exchange at multiple scales across key collisional/collisionless boundaries Interstellar Probe to characterize boundary regions of solar wind- interstellar medium interaction 3

4. F1C:Identify key processes that couple regions from solar and planetary atmospheres to the heliosphere and beyond. Required Understanding How do scale sizes change across boundaries? To elucidate cross-scale coupling in all regions from the Sun through the Earth’s atmosphere and into interplanetary space What is the role of shocks, wave-wave and wave-particle interactions in coupling? What are the important scale sizes for coupling in the solar atmosphere and the solar wind? What role does microturbulence play in coupling to very large scales? Transition from magnetically dominated to flow dominated processes Coupling occurs regardless of activity Incorporate PIZZO FOG Enabling Capabilities & Measurements Current and near future in-situ, and remote measurements and imaging from SEC Great Observatory In situ particle and field measurements on satellite clusters with variable spacing New simulation techniques to incorporate turbulence on a microscale into large-scale systems Multi-spacecraft ionospheric measurements and imaging combined with solar EUV and soft x-ray input High time resolution imaging of multiple layers in the solar atmosphere Wind and wave interactions in the ionosphere and mesosphere Implementation Phase 1: 2005-2015 Existing Assets Theory/Modeling Program To enable predictive capabilities at the Sun and Earth Cluster, STEREO, TIMED, L1/ Earth multi-measurementsTo elucidate solar wind cross-scale coupling and the change of scale sizes across boundaries. TIMED for elucidate winds, waves, and resulting interaction across temporal and spatial scales. Enabling STP Program Enabling LWS Program MMS To observe scale lengths of reconnection in situ and determine the importance of microturbulence SDO, IT Storm Probes + ITImager To determine the important scale size coupling in the solar atmosphere and to provide input for ionospheric ITImager is for thermospheric tidal structure Enabling Explorer Program Ground Observatories To enable predictive capabilities at the Sun and Earth IBEX Energetic neutral atoms to image our solar system’s previously invisible outer boundaries to discover how the solar wind interacts with the galactic medium and to reveal many of its unknown properties. Enabling STP GEC - Observe energy/momentum exchange at multiple scales across key collisional/collisionless boundaries 4

5. F2A: Understand the Magnetic Processes that Drive Space Weather 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, LWS FUV Imager Contributing LWS Program Enabling LWS missions ITSP – will provide understanding of ionospheric dynamo processesand coupling Sentinels – will provide the large scale system dynamics SWBuoys- define spatioal and temporal scales of CMEs and SPEs Potential Discovery Other Agencies Mission to provide a comparative magnetosphere to test understanding US: L1 Monitor Foreign: ORBITALS, Ravens, Solar Obiter Contributing STP Program Enabling STP Program Enabling GEC – will provide the ionospheric boundary conditions for reconnection Potential Explorer Flagship mission MagCon – will provide configuration of plasma and mag field for large scale mag system, provide information on acceleration and reconnection Mission to provide dynamics and topology of large scale magnetic system and coupling parameters Solar Probe – will provide obs of acceleration process near sun Required Understanding Critical parameters that determine coupling phenomena across multiscalar interfaces Dominant processes controlling reconnection and acceleration Source driver for solar/stellar and planetary dynamos Dynamics and topology of magnetospheres as a function of internal and external drivers How processes accessible in the Earth’s magnetosphere relate to other planetary magnetic systems Dynamics and topology of Sun and heliosphere as a function of internal and external drivers Creation and evolution of ionospheric dynamos Enabling Capabilities & Measurements Neutral wind and dynamo electric fields in the ionosphere Large scale observations of magnetically controlled phenomena Hybrid computer algorithms for complex cross-scale models Remote and in situ near-Sun particle and field observations Community access to system level Sun-Earth models Spatially and temporally resolved observations of multiscale interface regions Sun-Corona, SW-CME, SW-Mag, Mag-IT, IT-Atm, Helio-Interstellar Implementation Phase 2: 2015-2025 Model/Theory Development Community wide modeling workshops focusing on model development + Theory Program 5

6. 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/NES - quantify critical parameters for the source regions and the SEP outputs SWBuoys-characterize acceleration and injection histories of SEPs 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 Enabling Enabling Contributing STP Program STP Program STP Program Enabling Potential Explorer Flagship mission AAMP – mission to quantify the acceleration processes probing the readily available near Earth environment. GEC– measuresionospheric control of magnetospheric acceleration processes MagCon– meso-scale acceleration processes in the magnetosphere 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 MAD-pick up ion and dust acceleration Model/Theory Development - Community wide modeling workshops focusing on model development + Theory Program 6

7. F2C: Targeted Outcome: Understand nonlinear processes and coupling to predict atmospheric and space environments 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 Solar Probe, SEPP/NES, AAMP These are missions that also could provide critical measurements for understanding linkages between regions ITM-Waves, GEC, GEMINI, MC, Sentinels These are the most important missions in this phase to address coupling mechanisms at interfaces Heliostorm/L1 solar wind geospace coupling Mars Aeronomy and Dynamics interface between the upper and lower atmosphere at Mars 7

8. 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: Farside/SHIELDS - remote sensing Enhancing: Existing: MagCon; SWBuoys; GEMINI;Sentinels;SEPP/NES SPI /Telemachus- polar in-situ and remote Stellar Imager – dynamo context DBC: dayside magnetic structure Theory and Modeling: Predictability analysis of MHD systems and coupling to small scales IMC: inner magnetospheric dynamics RAM/MTRAP - coronal structure 8

9. F3B: Predict High Energy Particle Flux Throughout the Solar System Targeted Outcome: Phase 3- 2025-beyond, Opening the Frontier Great Observatory Assumes GEC, MagCon, , L1 monitor, SEPP, Auroral Imagers, Solar Sentinels, Contributing LWS Program Mission that remotely observes the solar source of particles and impact of particles in Geospace Inner Helio. Sentinels; SWBuoys: 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 Interstellar Probe - Measurements during cruise phase IMC-inner magnetospheric Enabling STP Program Enabling Potential Explorer Flagship mission Farside/Shields 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 9

10. 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 10