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Present and Future Research Directions and Space Missions for the Space Sciences Laboratory at Univ. of California, Berk

Explore the past and present missions of UC Berkeley's Space Sciences Laboratory, its research efforts, operational missions, and ongoing projects in collaboration with various agencies and organizations.

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Present and Future Research Directions and Space Missions for the Space Sciences Laboratory at Univ. of California, Berk

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  1. Present and Future Research Directions and Space Missions for the Space Sciences Laboratory at Univ. of California, Berkeley R. P. Lin Physics Department & Space Sciences Laboratory University of California, Berkeley

  2. SPACE SCIENCES LABORATORY • (UC Berkeley Organized Research Unit) • Background • Initiated in 1958 by Drs. Teller and Seaborg • Multidisciplinary organization • Connecting campus research to space efforts • Facility opened in 1966 • New facilities added in 1998 • Research Efforts Involving • Balloons • Sounding rockets • Satellite instruments & science complements • Complete satellites & multi-satellite missions • Mission & Science Operations • Ground Station Operations • Agencies Involved • NASA, NSF, NSBF, USAF, DOE • ESA, ISAS, IKI, PSI, etc. • $30-50M/yr (>90% NASA, <10% other.)

  3. Operational Missions & Instruments THEMIS – 5 S/C MIDEX mission RHESSI SMEX mission FAST SMEX mission STEREO 2 S/C - IMPACT & SWAVES Wind 3DP Cluster -4 S/C EFW, CIS ROCSAT 2 - ISUAL GALEX detectors SOHO UVCS & SUMER detectors Under Development HUBBLE - COS RBSP – E-fields Nu-STAR MAVEN Under Study NICE SMEX mission JDEM SNAP TARANIS XGRE CINEMA

  4. Operations Components • Mission Operations Center • Science Operations Center • 11-meter S-Band Antenna with • X-band capability • High Speed Communications to NASA • Ground Network • Network Security • Autonomous Operations • Pass Supports • Orbit Determination & Tracking • Spacecraft Command & Control • Emergency Response System • Self Checking

  5. SSL PERSONNEL 94 Scientific Researchers/Post-Docs/Visiting Scholars 127 Professional/Technical/Support Staff 30-40 Graduate students & 80-100 Undergraduate Students

  6. FAST • (Fast Auroral SnapshoT) • Science Package • Electric Field Instruments • Particle Instruments • Electronics • Mission Operations • Science Operations • Launched on 21 Aug 1996 • Mission Presently Operating

  7. RHESSI • (Ramaty High Energy Solar Spectroscopic Imager) • Project Management • Spacecraft Bus • Science Package • Imager • Spectrometer • Electronics • Mission Operations • Science Operations • Ground Data Systems • Launched February 5, 2002 • Mission presently operating

  8. THEMIS TIME HISTORY OF EVENTS AND MACROSCALE INTERACTIONS DURING SUBSTORMS RESOLVING THE MYSTERY OF WHERE, WHEN AND HOW AURORAL ERUPTIONS START Dr. Vassilis Angelopoulos, PI

  9. THEMIS Integration and Test • 5 identical spacecraft & instrument suites

  10. UC Berkeley Space Sciences Laboratory IMPACT Investigation on NASA’s STEREO (Solar Terrestrial Observatory) Mission Dr. Janet Luhmann (PI) http://www.nasa.gov/stereo http://sprg.ssl.berkeley.edu/impact

  11. + X + Z - Y + Y - Z - X Low Gain RF Antenna (2) (LGA) SECCHI Sun-Centered Imaging Package (SCIP) Assy (COR-1, COR-2, EUVI, GT) Adapter Ring Inertial Measurement Unit (IMU) Bi-fold Solar Panel PLASTIC Instrument Sun Sensor (5) Deployed High Gain RF Antenna (HGA) IMPACT SEP Deployed SWAVES Electric Field Antenna (3 places) SECCHI Heliospheric Imager (HI) Deployed IMPACT Boom IMPACT Magnetometer (MAG) IMPACT Suprathermal Electrons (STE) IMPACT Solar Wind Electron Analyzer (SWEA)

  12. Electric Field Instrument (J. Wygant U. Minnesota, PI); J. Bonnell SSL , Project Scientist

  13. BARREL Balloon Array for RBSP Relativistic Electron Precipitation R. M. Millan, PI Dartmouth College

  14. NCT (Nuclear Compton Telescope) S. Boggs , PI

  15. Mars Atmosphere and Volatile EvolutioN (MAVEN) Mission PI: Bruce Jakosky U. Colo. LASP Dep. PI: Bob Lin, UC Berkeley SSL Lockheed-Martin spacecraft

  16. MAVEN Will Measure the Drivers, Reservoirs, and Escape Rates • MAVEN will determine the present state of the upper atmosphere and today’s rates of loss to space. • Essential measurements allow determination of the net integrated loss to space through time.

  17. NICE (Neutral Ion Coupling Explorer) S. Mende, PI PI

  18. SNAP • (SUPERNOVA ACCELERATION PROBE) • Professor S. Perlmutter, Dr. M. Levi • LBNL/SSL Collaboration • Project Management • Spacecraft Bus • 2m Telescope • Integration and Test • Mission Operations • Ground Data Systems

  19. October 27, 2002 size CME velocity ~2000 km/s very large source (>200 arcsec) expanding and rising motion 300” 800 km/s

  20. RHESSI and GOES GOES in LINEAR scale! GOES background B6 microflares: A6 or smaller At least 7 microflares Spectrogram plot: time-energy, colors represent counts

  21. RHESSI Microflare spatial distribution(Christe et al., 2008) • Micro

  22. FOXSI (Focussing Optics hard X-ray Spectrometer Imager) FOXSI (Focussing Optics for hard X-ray Spectroscopy & Imaging) S. Krucker, PI

  23. Protons vs>~30 MeV p (2.223 MeV n-capture line)> 0.2 MeV e (0.2-0.3 MeV bremsstrahlung X-rays)e & p separated by ~104 km, but close to flare ribbons

  24. GRIPS(Gamma-Ray Imaging Polarimeter for Solar r Flares) R. Lin, PI

  25. !. RHESSI Terrestrial Gamma-ray Flashes:

  26. XGRE instrument on French (CNES) TARANIS mission

  27. Wind observations of the ion diffusion region (Xgsm = - 60 Re) (Øieroset et al., Nature, 2001) Wind NP Flow reversal VX Earthward jets Tailward jets BX Continuous Vx reversal Bz reversal Hall magnetic field observed in 3 out of 4 quadrants ~4 nT Hall magnetic field (40%) ~6 nT guide field (50%) Hall magnetic fields BY BZ

  28. Wind Electron energization up to 300 keV inside the diffusion region (Øieroset et al., PRL, 2002) Peak of electron energization inside the diffusion region Energization up to ~300 keV Not predicted by theory! NP VX electrons ions B Diffusion region could be a direct source of high-energy electrons in the Earth’s plasma sheet

  29. ARTEMIS ARTEMIS “Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon’s Interaction with the Sun”

  30. Acceleration in shocks, tail and lunar environment • What is the nature of acceleration at shocks? • Follow evolution of particle distributions at two points along the shock. • How do MeV electrons get accelerated in the tail? • Measure field topology, particle spectra and evolution in time and space. • How do energetic (100s of keV) ions and electrons get accelerated in the wake? • Measure particles and fields in the wake and the solar wind simultaneously. • Reconnection • What is the distant tail reconnection onset mechanism, effects and response to solar wind drivers? • Spontaneous or induced? • Continuous or impulsive? • Answers necessitate multiple THEMIS-type satellites at 1-20RE scales • Lunar Wake (after Lunar Prospector and WIND) • What are the plasma waves that make up the nature of the Lunar Wake? • How does the wake fill-in from near the moon to far down • What makes up, sustains and dissipates the electric fields behind the wake • Measure particles and fiels in the wake and outside at 1000-50,000km distance

  31. The SupraThermal Electron (STE) sensor on STEREO is the first silicon semiconductor detector in space to detect particles to <~2keV T Sun D2 D1 R D0 STE D3 Energetic neutral atoms (ENAs) will be detected as ions since they will be ionized upon passing through the detector window.

  32. Major peak: γ1~2.8 below the break (~10-12keV) γ2~5.6 above Minor peak: γ1~2.5 below γ2~5.4 above Nose

  33. Termination shock IS Wind Solar wind LISM Sun Heliosphere ENA ISN ion Heliosheath Heliopause Bow shock

  34. Wang et al., Nature , 2008 ENA at 1 AU Major peak Minor peak

  35. 2006 November 6 Terrestrial ENA observations Sun X STE-U Y Z Earth STE-D

  36. Average particle energy spectra

  37. Inferred source proton energy spectra

  38. CINEMA (Cubesat for Ion, Neutral, Electron, MAgnetic fields)

  39. Sun X STEREO A Y Z Earth STEREO B A B Earth 2007 January Anomalous ENA Observations

  40. STEREO B

  41. STB Detector looking direction (source direction) in GSE coordinate 15 keV Moon Earth No background removal

  42. Background-subtracted flux

  43. Source protons Gruntman, 1997 jENA= jp× L × (σpH×nH + σpHe×nHe) but at ~ 1 AU, nHe = 0.015 cm-3 and nH ~ 0

  44. Interstellar neural helium is present throughout the heliosphere and beyond (except very close to the Sun, <~0.3 AU). Interstellar hydrogen dominates outside of ~3 AU, and near planets. Imaging of suprathermal (~few to >~30 keV) ions throughout the heliosphere and beyond, is possible with sensitive instrumentation to detect the ENAs from charge exchange with interstellar helium & hydrogen

  45. Universities Involvement in Space SciencesExcellence in ScienceInnovation in TechnologyStudent Training Efficiency (Cheap)

  46. Opportunities: Small/Medium Class Missions – SMEX, MIDEX, Discovery, Mars Scout, New Frontiers, Venture/ESSPs International collaborative missions Instruments on Larger Missions Rocket & Balloon-borne Projects (& Cubesats)

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