1. Targeted Outcome: Phase 2005-2015, Opening the Frontier Characterize magnetic reconnection at the Sun and the Earth F1A: Targeted Outcome to Capabilities to Implementation 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 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 Implementation Phase 1: 2005-2015 Required Understanding What mechanisms lead to onset of reconnection? What are the mechanisms and regions of particle acceleration within the reconnection geometry? Where are the reconnection regions and what is their topology? What instabilities lead to global effects? To elucidate the role of microphysics, meso-scales, global topology and cross- scale coupling in reconnection THEMIS - substorm dynamics Solar B - solar magnetic fields STEREO- CMEs RBSP- particle acceleration SDO - solar magnetic variability and large scale, structure RHESSI - 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 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 Complementary missions to study precursors or results of reconnection Explorer Candidates L1 Monitor - to provide solar wind conditions Auroral Imaging - to monitor substorm onsets and energy dissipation Other Agencies Enabling STP mission High resolution imaging multiple wavelengths to measure dynamics of magnetic fields from photosphere through corona

2. F1B: Determine the Dominant Processes of Particle Acceleration Phase 2005-2015, Open the Frontier 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 Enabling Capabilities & Measurements Implementation Phase 1: 2005-2015 Required Understanding Shock acceleration processes Role of magnetic field topology Waves, turbulence & intermittent processes Coherent electric field acceleration Output Energy Spectrum and Composition Primary acceleration sites: - Coronal Mass Ejection Shocks - Solar flares, Current Sheets - Bow shocks, Radiation Belts - Magnetotails, Auroral Zones - Termination Shock 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 Role of seed particle population MMS- acceleration in reconnection STEREO, Solar-B For acceleration at CME/flare sites Stochastic acceleration processes Thermal plasma (solar wind) 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 Multi-point In-situ measurements of density, temperature, velocity, energy spectrum, and charge state of particles; and electric/magnetic fields at coronal & heliospheric shocks Multi-point in-situ determinations of mag- netospheric energetic particles & fields at micro/meso-scales Visible light Coronagraph/ Polarimeter for electron density evolution and flow speeds Near-Sun measurements of neutrons, hard X-rays & gamma rays Neutral Energetic Ion Imaging of Termination Shock THEMIS, IBEX Explorer Missions for particle acceleration at I/F Existing Assets Explorer ProgramContributing SDO For acceleration at CME/flare sites IT-Imager; GEC Role of ionospheric conductivity for auroral acceleration STP ProgramEnablingLWS ProgramContributingLWS ProgramEnabling NESCE [Near-Earth Solar Coronal Explorer] Characterize SEP coronal source regions & emissions Potential ExplorerEnabling 2 High alt rocket-lower alt auroral acceleration

3. F1C: Identify key processes that couple regions from solar and planetary atmospheres to the heliosphere and beyond Current and near future in-situ, and remote measurements and imaging from SEC Great Observatory Enabling Capabilities & Measurements New simulation techniques to incorporate turbulence on a microscale into large-scale systems Implementation Phase 1: 2005-2015 Required Understanding Role of turbulence in coupling to very large scales Important scale sizes for coupling in the solar atmosphere and the solar wind? Change of scale sizes across boundaries To elucidate cross-scale coupling in all regions from the Sun through the Earth’s atmosphere and into interplanetary space Cluster, STEREO, TIMED, L1/ Earth multi-measurements To 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 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 Theory/Modeling Program To enable solar, heliospheric and geospace modeling to understand couplings High time resolution imaging of multiple layers in the solar atmosphere Multi-spacecraft & cluster ionospheric/ magnetospheric in situ measurements and imaging combined with solar EUV and soft x-ray input LWS ProgramEnabling STP ProgramEnabling IBEX I to image heliospheric boundaries; ISP to characterize boundary regions of solar wind- interstellar medium interaction Explorer ProgramEnabling Role of shocks, wave-wave and wave- particle interactions in coupling Wind and wave interactions in the ionosphere and mesosphere SPI/Telemachus to observe solar wind structure and high latitudes SWB to observe solar wind structure at all longitudes Existing Assets GEC - Observe energy/momentum exchange at multiple scales across key collisional/collisionless boundaries STP Enabling Transition from magnetically dominated to flow dominated processes 3 Evolution of emerged solar magnetic flux under coupled interaction between differential rotation and small-scale fluid and plasma transport mechanisms Generation, transport, and evolution of solar open flux regions coronal magnetic field measurements & helioseismology 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 Deep-space observations of heliospheric boundary Interstellar Probe to characterize boundary regions of solar wind- interstellar medium interaction

4. F1C: Identify key processes that couple regions from solar and planetary atmospheres to the heliosphere and beyond. In situ particle and field measurements on satellite clusters with variable spacing Current and near future in-situ, and remote measurements and imaging from SEC Great Observatory Enabling Capabilities & Measurements New simulation techniques to incorporate turbulence on a microscale into large-scale systems Implementation Phase 1: 2005-2015 Required Understanding What role does microturbulence play in coupling to very large scales? What are the important scale sizes for coupling in the solar atmosphere and the solar wind? 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 Cluster, STEREO, TIMED, L1/ Earth multi-measurements To 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. 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 Theory/Modeling Program To enable predictive capabilities at the Sun and Earth High time resolution imaging of multiple layers in the solar atmosphere Multi-spacecraft ionospheric measurements and imaging combined with solar EUV and soft x-ray input LWS ProgramEnablingSTP ProgramEnabling 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. Explorer ProgramEnabling What is the role of shocks, wave- wave and wave-particle interactions in coupling? Wind and wave interactions in the ionosphere and mesosphere Ground Observatories To enable predictive capabilities at the Sun and Earth Existing Assets Coupling occurs regardless of activity Incorporate PIZZO FOG GEC - Observe energy/momentum exchange at multiple scales across key collisional/collisionless boundaries STP Enabling Transition from magnetically dominated to flow dominated processes 4

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

6. F2B: Quantify Particle Acceleration for Key Regions of Exploration Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction Enabling Capabilities & Measurements Implementation Phase 2: 2015-2025 Required Understanding Identify dominant processes controlling stochastic acceleration 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 Remote and in situ particle and field observations of the corona and near- Sun acceleration regions Spatially and temporally resolved observations of shock interface in key regions (Sun-Corona, SW-CME-CIR, CME-Mag, Helio-Interstellar) 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 Quantify the dynamics of magnetic topology and electric fields in key regions Model/Theory Development - Community wide modeling workshops focusing on model development + Theory Program SEPP/NES - quantify critical parameters for the source regions and the SEP outputs SWBuoys-characterize acceleration and injection histories of SEPs LWS missionsEnabling Sentinels – will observe heliospheric acceleration shock regions created by CMEs LWS ProgramContributing US: L1 Monitor, ATST Foreign: ORBITALS, Ravens, Solar Obiter Other Agencies Mission to observe and quantify acceleration processes associated with electric field in a magnetized environment Potential Explorer AAMP – mission to quantify the acceleration processes probing the readily available near Earth environment. STP ProgramEnabling Assumes launch of Solar-B, MMS, SDO, RBSP, THEMIS, IBEX, Cluster, ITSP, L1 monitor Great Observatory Mission to observe in situ and quantify interplanetary acceleration processes at shock boundaries Potential Discovery Solar Probe – will provide obs of acceleration process near sun Flagship mission Enabling Production and distribution of the seed particles (pickup ions, suprathermal plasmas in the solar corona and planetary magnetospheres) that are accelerated to high energies 6 MagCon– meso-scale acceleration processes in the magnetosphere STP ProgramEnabling GEC– measures ionospheric control of magnetospheric acceleration processes STP ProgramContributing MAD-pick up ion and dust acceleration

7. F2C: Targeted Outcome: Simultaneous, colocated neutral winds, ionospheric densities & drifts Global characterization of the current systems linking geospace using swarms of satellites Enabling Capabilities & Measurements Multi-point measurements of solar wind and dayside magnetopause Implementation Phase 2: 2015-2025 Required Understanding Transfer of solar wind information through planetary electrodynamic systems Detailed coupling of magnetotail dynamics to the polar region Transition of solar steady and eruptive events from interior of the sun to the atmosphere Feedback of the ionosphere on magnetospheric electrodynamics 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/NES, AAMP These are missions that also could provide critical measurements for understanding linkages between regions Theory/Modeling Coupled models between regions of space to provide physical insight on mass and energy transfer rates Two-way-coupled modeling capabilities Simultaneous multi-point characterization of the magnetotail and imaging of the auroral oval Chemical & dynamical coupling between upper atmosphere disturbances & the lower atmosphere Simultaneous measurement of solar reconnection features and heliospheric density structures Satellite observations of atmospheric chemistry & key dynamical features Controllers of mass and energy flow between the solar wind and geospace Meteorological Forcing of the ITM Global I-T coupling and the creation of instabilities Mars Aeronomy and Dynamics interface between the upper and lower atmosphere at Mars 7 Understand nonlinear processes and coupling to predict atmospheric and space environments Heliostorm/L1 solar wind geospace coupling

8. F3A: Predict Solar System Magnetic Activity and Energy Release Targeted Outcome: 2025-beyond, Opening the Frontier Integrated MHD/plasma models of coronal magnetic heating and stability Whole-Sun remote-sensing observations (magnetic, velocity, XUV, EUV) Enabling Capabilities & Measurements Integrated solar interior- atmosphere magnetic models using observational inputs Implementation Required Understanding Dominant processes controlling solar dynamo Characterize predictability of dynamo: analytic, statistical, or chaotic 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 Farside/SHIELDS - remote sensing RAM/MTRAP - coronal structure Stellar Imager – dynamo context Theory and Modeling: Predictability analysis of MHD systems and coupling to small scales Active region coronal measurements of magnetic field, velocity, thermal fine structure Characterize predictability of magnetic energy release Global heliosphere in-situ observations (plasma, field, particles) Production of paleoclimate tracers of solar activity Enabling: SPI /Telemachus- polar in-situ and remote Enhancing: 8 Understand to the level of predictability the ionospheric dynamo Measurements throughout the magnetosphere of fields and particles Measurements throughout the ionosphere and thermosphere of density, comp. and drifts MagCon; SWBuoys; GEMINI;Sentinels;SEPP/NES IMC: inner magnetospheric dynamics DBC: dayside magnetic structure Existing:

9. F3B: Predict High Energy Particle Flux Throughout the Solar System Targeted Outcome: Phase 3- 2025-beyond, Opening the Frontier Enabling Capabilities & Measurements Implementation Phase 3: 2025-beyond Required Understanding Understand the source of dominant processes that create energetic particles at the Sun, in interplanetary space and within magnetospheres Understand the energization processes across multiscalar interfaces that result in acceleration of particles 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 Understand transport processes of energetic particles in interplanetary regions in the Solar System Model/Theory Development - Theory and Modeling program focused on predicting particle flux and populations throughout the Solar System Inner Helio. Sentinels; SWBuoys: Solar wind mission that quantifies particle fluxes within 1 AU and within Geospace Mission that remotely observes the solar source of particles and impact of particles in Geospace LWS ProgramContributing US: monitor of geoeffective solar phenomena (chronograph?) Other Agencies Mission to quantify the dynamics of and particle interaction across the heliospheric boundary Potential Explorer IMC-inner magnetospheric STP ProgramContributing Farside/Shields STP ProgramEnabling Assumes GEC, MagCon,, L1 monitor, SEPP, Auroral Imagers, Solar Sentinels, Great Observatory Mission to observe quantify Mercury’s magnetospheric particle and plasma populations Potential Discovery Mission to quantify the particle and energy propagation through the solar wind-magnetosphere-ionosphere system IMC, MagCon, DBC, AAMP Flagship mission Enabling From Phase 2: Understand SW magnetic processes and quantify acceleration in key regions Remote and in situ observations in Geospace and other planetary magnetospheres in order to predict particle fluxes Determine the plasma populations throughout the Solar System 9 Interstellar Probe - Measurements during cruise phase ??? ProgramContributing Understand the transfer of energetic particles between regions of space (e.g., heliosphere to magnetosphere)

10. F3C: Understand the Interactions of Disparate Astrophysical Systems Targeted Outcome: Phase 3- 2025-beyond, Open the Frontier Determine isotopic and elemental composition, flow directions, speed, and temperature of pickup ions and neutrals with in-situ stellar probes Image heliopause Enabling Capabilities & Measurements Solar sail technology to enable interstellar spacecraft Implementation Phase 3: 2025-2035 Required Understanding The location and 3D structure of the interaction region between the heliosphere and local galactic environment Cosmic ray interaction with 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 Heliospheric Imager & Galactic Observer (HIGO) To image the interaction between interstellar medium and heliopause 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 Measure low-energy cosmic rays in situ with interstellar probes Image termination shock using energetic hydrogen atoms and radio detection 10 Understand to the level of prediction the coupling between interplanetary medium and magnetosphere- ionosphere-atmosphere system Multipoint measurements of SW- magnetosphere coupling In situ and remote measurements of magnetosphere-ionosphere coupling Measurements of coupling between atmospheric layers/regions DBC, MagCon, IMC Constellations to investigate SW- magnetospheric coupling TITM-C, ITM-Waves, AAMP Missions to quantify atmospheric coupling