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Solar Probe Plus A NASA Mission to Touch the Sun Solar Probe Plus – A Mission to Touch the Sun Rob Decker and Nicky Fox Johns Hopkins Applied Physics Laboratory.

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Presentation on theme: "Solar Probe Plus A NASA Mission to Touch the Sun Solar Probe Plus – A Mission to Touch the Sun Rob Decker and Nicky Fox Johns Hopkins Applied Physics Laboratory."— Presentation transcript:

1 Solar Probe Plus A NASA Mission to Touch the Sun Solar Probe Plus – A Mission to Touch the Sun Rob Decker and Nicky Fox Johns Hopkins Applied Physics Laboratory Laurel, Maryland, USA Representing SPP Project and Science Investigation Teams 1

2 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Solar Probe History (1958 - present) Solar Probe studies, reports; NAS: 1962, 1985, 1995, 2003; 2013 2 European Solar Physics 14

3 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Science Questions Addressed by Solar Probe Plus OVERARCHING SCIENCE OBJECTIVE  To determine the structure and dynamics of the Sun’s coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what mechanisms accelerate and transport energetic particles. Detailed Science Objectives  Trace the flow of energy that heats and accelerates the solar corona and solar wind.  Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind.  Explore mechanisms that accelerate and transport energetic particles.  Level 1 Mission and Measurement Requirements have been derived in order to achieve these science objectives  There are three detailed science sub-questions stemming from each objectives …. 3

4 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Detailed Science Sub-Questions  Trace the flow of energy that heats and accelerates the solar corona and solar wind.  How is energy from the lower solar atmosphere transferred to, and dissipated in, the corona and solar wind?  What processes shape the non-equilibrium velocity distribution observed throughout the heliosphere?  How do the processes in the corona affect the properties of the solar wind in the heliosphere?  Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind.  How does the magnetic field in the solar wind source regions connect to the photosphere and the heliosphere?  Are the sources of the solar wind steady or intermittent?  How do the observed structures in the corona evolve into the solar wind?  Explore mechanisms that accelerate and transport energetic particles.  What are the roles of shocks, reconnection, waves, and turbulence in the acceleration of energetic particles?  What are the source populations and physical conditions necessary for energetic particle acceleration?  How are energetic particles transported in the corona and heliosphere? 4

5 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 SPP Investigations to Answer the Science Questions InvestigationInstrumentsPrinciple Investigator Fields Experiment (FIELDS) 4 x Electric Antennas (+ 1 probe on mag boom) 2 x Fluxgate Magnetometer (MAG) 1 x Search Coil Magnetometer (SCM) Prof. Stuart D. Bale, University of California Space Sciences Laboratory, Berkeley, CA Integrated Science Investigation of the Sun (ISIS) High energy Energetic Particle Instrument (EPI-Hi) Low energy Energetic Particle Instrument (EPI-Lo) Dr. David J. McComas, Southwest Research Institute, San Antonio, TX Solar Wind Electrons Alphas and Protons (SWEAP) Solar Probe Faraday Cup (SPC) 2 Solar Probe ANalyzers (SPAN; ESAs) Dr. Justin Kasper, University of Michigan, Ann Arbor, MI & Smithsonian Astrophysical Observatory, Cambridge, MA Wide-field Imager for Solar PRobe (WISPR) White light imagerDr. Russ Howard, Naval Research Laboratory, Washington, DC Heliospheric Origins with Solar Probe Plus (HeliOSPP) Observatory Scientist: Addresses SPP science objectives via multi-instrument data analysis to optimize the scientific productivity of the mission Dr. Marco Velli, Jet Propulsion Laboratory, Pasadena, CA 5

6 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Level 1 Objectives & Processes Require High-quality, Integrated Measurements L1 Science Objectives Sample Processes Needed Measurements Instruments 1. Trace the flow of energy that heats and accelerates the solar corona and solar wind. 2. Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind. 3. Explore mechanisms that accelerate and transport energetic particles. - heating mechanisms of the corona and the solar wind; - environmental control of plasma and fields; - connection of the solar corona to the inner heliosphere. - particle energization and transport across the corona - electric & magnetic fields and waves, Poynting flux, absolute plasma density & electron temperature, spacecraft floating potential, & density fluctuations, & radio emissions - energetic electrons, protons and heavy ions - velocity, density, and temperature of solar wind e-, H+, He++ - solar wind structures and shocks FIELDS -Magnetic Field -Electric Field -Electric/Mag Wave ISIS -Energetic electrons -Energetic protons and heavy ions -(10s of keV to ~100 MeV) SWEAP -Plasma e-, H+, He++ -SW velocity & temperature WISPR - White light measurements of solar wind structures (add context) 6

7 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Reference Vehicle: Anti-Ram Facing View 7

8 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Reference Vehicle: Ram Facing View 8

9 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Particle Instrument capabilities meet Level 1 requirements with margin electrons protons ions helium 1eV1keV1MeV1GeV Energy (log) L1 Requirement SWEAP-SPC ISIS-EPI-Lo SWEAP-SPAN SWEAP-SPC SWEAP-SPAN ISIS-EPI-Lo ISIS-EPI-Hi Particle Sensors SWEAP/SPAN SWEAP/SPC ISIS/EPI-Lo ISIS/EPI-Hi 9

10 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Fields & Waves Instrument capabilities meet Level 1 requirements with margin Frequency (log) Fields & Waves Sensors FIELDS/FGM FIELDS/SCM FIELDS/EFI FIELDS/PWI ~DC 10Hz1kHz1MHz DC Magnetic DC Electric AC Magnetic Plasma Waves Radio Quasi-thermal Noise FIELDS FGM FIELDS EFI FIELDS PWI FIELDS SCM FIELDS PWI L1 Requirement 10

11 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Reference Mission: Launch and Mission Design Overview Launch  Dates: Jul 31 – Aug 19, 2018 (20 days)  Max. Launch C3: 154 km 2 /s 2  LV will be a Delta 4 Heavy or Falcon Heavy (Space News, 25 Jul 2014) Trajectory Design  7 Venus gravity assist flybys Final Solar Orbits  Perihelion: 9.86 R S  Aphelion: 0.73 AU  Inclination: 3.4° from ecliptic  Orbit period: 88 days Mission duration: 7 years Sun Venus Mercury Earth Launch 7/31/2018 1st Min Perihelion at 9.86 R S 12/19/2024 1st Perihelion at 35.7 R S 11/1/2018 11

12 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 SPP Rapidly Explores the Inner Heliosphere  1 st perihelion (0.16 AU) 3 months after launch  24 passes below 43 Rs  19 passes below 20 Rs 12

13 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 0.25 A.U. Cruise/Downlink Period 24 Solar Encounter Orbits Orbital Periods Vary (168 days to 88 days) Encounter Operations  Primary science data collection phase – All instruments will be powered on  Fanbeam antenna periodically available for communications & Nav  No SSR Playbacks Orbital Operations Concept Cruise Operations  Instruments Can Be Powered On (Sun Distance < 0.82 AU)  Instruments off during some activities  Fanbeam for communications – H/K data only  Commanding as needed to support spacecraft maintenance Science Downlink Operations  All instruments powered off  HGA for communications – SSR playbacks  Commanding as needed to support spacecraft maintenance Solar Encounter Period Cruise/Downlink Period Solar Encounter Period (10-11 days) 13 0.25 A.U.

14 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Reference Vehicle: Concept of Operations 14

15 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 Solar Cycle: SPP will be going from minimum to ascending phase? Cycle 25 ?? 2025

16 Solar Probe Plus A NASA Mission to Touch the Sun European Solar Physics Meeting 14 08 Sep 2014 It has been 50+ years since the Solar Probe Concept was introduced... Solar Probe Plus, currently in mid Phase C, is moving along! 16

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