Virtual Energetic Particle Observatory: Enhancing Heliophysics Research

1. The Global Heliophysics Observatory for IPY – IHY, 2007 - 2009 John F. Cooper Chief Scientist, Space Physics Data Facility Heliospheric Physics Laboratory NASA Goddard Space Flight Center Greenbelt, Maryland, U.S.A.

2. The Heliophysics Great Observatory Geosynchronous Satellites THEMIS Wind Geotail Stereo IMAGE SOHO RHESSI ACE Solar Source Cluster Polar Solar Wind Drivers FAST Seed Population TIMED Precipitation And Loss Atmospheric & Ionospheric Coupling Inner Heliosphere Outer Heliosphere Ulysses Voyager 2 New Horizons Local Interstellar Medium Planetary Interactions Heliosheath Voyager 1, 2 (2008?) IBEX (2008) Mercury/Messenger Mars Missions Cassini/Saturn-Titan Telescopes GCR Balloons IBEX (2008) Ground-based Instruments

3. Heliophysics - Space Physics Environments Heliosphere of Sun to Planets and the Local Interstellar Medium

4. The Heliospheric Network TS-crossing Dec. 16, 2004 IBEXLaunch June 15, 2008

5. THEMIS NEW HORIZONS CASSINI

8. VEPO Data Environment Could Expand to Cosmic Ray Balloon Experiments Balloon-borne Experiment with a Superconducting Spectrometer (BESS) BESS-Polar 2004, 2007+ Antarctic Flights Ep > 100 MeV

9. Neutron Monitors are Ancillary VEPO Data Sources

13. CDAWeb Plus (An ACE Example)

14. CDAWeb Plus (A Voyager Example)

15. NNH06ZDA001N-VOBS: Virtual Observatories for Heliophysics DataVirtual Energetic Particle Observatory (VEPO)In Search of Dragon Fire John F. Cooper, Robert E. McGuire, Nand Lal, Adam Szabo, Thomas W. Narock NASA Goddard Space Flight Center, Greenbelt, Maryland Matthew E. Hill Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryand Thomas P. Armstrong, Jerry W. Manweiler Fundamental Technologies, Lawrence, Kansas Robert B. McKibben, Clifford Lopate University of New Hampshire, Durham, New Hampshire Contact: Dr. John F. Cooper, Heliospheric Physics Laboratory, Code 672, NASA Goddard Space Flight Center, Greenbelt, MD 20771 E-mail: John.F.Cooper@nasa.gov; Phone: +1-301-286-1193

16. Challenges of Heliophysics Energetic Particle Environment • Suprathermal (keV-MeV) and higher energy (MeV – GeV) energetic particles (EP) pervade heliospheric and planetary magnetospheric regions from solar, heliospheric, planetary (Jovian e−), and galactic sources • EP and related cosmic ray research has many cross-disciplinary science applications in earth science, heliophysics, and astrophysics; e.g. ionization rates in planetary atmospheres, carbon radioisotope dating for archeology • There is high demand for EP data as expressed by participants in U.S. and international science forums (AGU, EGS, COSPAR, AOGS, ICRC, etc) hosting EP-related sessions • Many sources of EP data relevant to heliophysics research currently exist from instruments of the operational and legacy Heliospheric Network spacecraft fleet and from ground-based and high-altitude balloon platforms • Investigations of origins, transport, and interactions of EP require analysis of multi-sensor, multi-spacecraft data sets from diverse repositories in varied formats and with varying degrees of documentation for usability and validation • A common view of EP environments in the Earth-Moon geospace system and for interplanetary journeys to Mars and beyond is needed for radiation hazard modeling, assessment, and mitigation in support robotic and human missions for the NASA Vision for Space Exploration • Virtual observatories and SPASE have largely not fully addressed special characteristics and challenges of EP in the heliophysics data environment

17. What is a Virtual Observatory, according to NASA? • “A Virtual Observatory (VO) is a suite of software applications on a set of computers that allows users to uniformly find, access, and use resources (data, software, document, and image products and services using these) from a collection of distributed product repositories and service providers. A VO is a service that unites services and/or multiple repositories.” • The Seven Pillars of Wisdom* for ViCRO Functions as a VxO • 1. Coordinated Discovery and Access • 2. Understanding of Data Needs • 3. Standards and Metadata • 4. APIs and Web services • 5. Value Added Services • 6. Ancillary Data Access • 7. Usage Assessment and Provenance Protection • *Wisdom hath builded her house, she hath hewn out her seven pillars (Proverbs 9:1)

18. The Seven Pillars of VEPO 1. Coordinated Discovery and Access 2. Understanding of Data Needs 3. Standards and Metadata 4. APIs and Web Services 5. Value Added Services 6. Ancillary Data Access7. Usage Assessment and Provenance Protection Wadi Rum, Jordan Reduced or deferred priorities on selected (e.g., planetary mission) existing data sets, and on value-added development of new intercalibrated data sets and OMNI-EP data system.

19. VEPO will mainly utilize VHO existing middleware VEPO-VHO Interface Development Team: T. W. Narock, R. E. McGuire et al. • Connection to processing services. • Connection to other VxOs

20. Virtual Heliospheric Observatory (VHO) 8 Spacecraft - 13 Data Sets • ACE • Magnetometer • SWEPAM IMP 8 - Magnetometer WIND - MFI - SWE - ELPD - PLSP • Genesis • Mag. Field Proxy • 3D Moments SOHO - Celias instrument • Helios 1 and 2 • Magnetometer • Plasma instrument • Mars Global Surveyor • Solar Wind Pressure Proxy SH43B-02 (4)

21. APL – Applied Physics Lab./JHU, FunTech = Fundamental Tech., HPL – Heliospheric Physics Lab./GSFC Green = high priority, Blue = medium priority, Red = deferred priority