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

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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

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• 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 (gt90 NASA, lt10 other.)

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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
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• 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

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SSL PERSONNEL 94 Scientific Researchers/Post-Docs/
Visiting Scholars 127 Professional/Technical/Suppo
rt Staff 30-40 Graduate students 80-100
Undergraduate Students
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• FAST
• (Fast Auroral SnapshoT)
• Science Package
• Electric Field Instruments
• Particle Instruments
• Electronics
• Mission Operations
• Science Operations
•  
• Launched on 21 Aug 1996
• Mission Presently Operating

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• 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

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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
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• THEMIS Integration and Test
• 5 identical spacecraft instrument suites

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UC Berkeley Space Sciences Laboratory IMPACT
Investigation on NASAs STEREO (Solar
Terrestrial Observatory) Mission Dr. Janet
Luhmann (PI)

http//www.nasa.gov/stereo http//sprg.ssl.berke
ley.edu/impact
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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)
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Electric Field Instrument (J. Wygant U.
Minnesota, PI) J. Bonnell SSL , Project Scientist
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Balloon Array for RBSP Relativistic Electron
Precipitation
BARREL

• R. M. Millan, PI
• Dartmouth College

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NCT (Nuclear Compton Telescope) S. Boggs , PI
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Mars Atmosphere and Volatile EvolutioN (MAVEN)
Mission
PI Bruce Jakosky U. Colo. LASP Dep. PI Bob
Lin, UC Berkeley SSL Lockheed-Martin spacecraft
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MAVEN Will Measure the Drivers, Reservoirs, and
Escape Rates

• MAVEN will determine the present state of the
  upper atmosphere and todays rates of loss to
  space.

• Essential measurements allow determination of
  the net integrated loss to space through time.

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

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October 27, 2002
size
CME velocity 2000 km/s
very large source (gt200 arcsec) expanding and
rising
motion
300
800 km/s
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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
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RHESSI Microflare spatial distribution(Christe
et al., 2008)

• Micro

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FOXSI (Focussing Optics hard X-ray Spectrometer
Imager)

• FOXSI (Focussing Optics for hard X-ray
  Spectroscopy Imaging) S. Krucker, PI

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Protons vsgt30 MeV p (2.223 MeV n-capture
line)gt 0.2 MeV e (0.2-0.3 MeV bremsstrahlung
X-rays)e p separated by 104 km, but close to
flare ribbons
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GRIPS (Gamma-Ray Imaging Polarimeter for Solar r
Flares) R. Lin, PI
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!.
RHESSI Terrestrial Gamma-ray Flashes
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XGRE instrument on French (CNES) TARANIS mission
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Wind observations of the ion diffusion region
(Xgsm - 60 Re) (Øieroset et al., Nature, 2001)
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
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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 Earths plasma sheet
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ARTEMIS Acceleration, Reconnection, Turbulence
and Electrodynamics of the Moons Interaction
with the Sun
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• 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

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The SupraThermal Electron (STE) sensor on STEREO
is the first silicon semiconductor detector in
space to detect particles to lt2keV
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.
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Major peak ?12.8 below the break (10-12keV)
?25.6 above Minor peak ?12.5 below ?25.4
above
Nose

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Termination shock
IS Wind
Solar wind
LISM
Sun
Heliosphere
ENA
ISN
ion
Heliosheath
Heliopause
Bow shock
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Wang et al., Nature , 2008
ENA at 1 AU
Major peak Minor peak
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2006 November 6 Terrestrial ENA observations
Sun
X
STE-U
Y
Z
Earth
STE-D
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Average particle energy spectra

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Inferred source proton energy spectra
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• CINEMA
• (Cubesat for Ion, Neutral, Electron, MAgnetic
  fields)

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

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STB Detector looking direction (source
direction) in GSE coordinate 15 keV
Moon
Earth
No background removal
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Background-subtracted flux
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Source protons
Gruntman, 1997
jENA jp L (spHnH spHenHe)
but at 1 AU, nHe 0.015 cm-3 and nH
0
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Interstellar neural helium is present throughout
the heliosphere and beyond (except very close to
the Sun, lt0.3 AU). Interstellar hydrogen
dominates outside of 3 AU, and near planets.
Imaging of suprathermal (few to gt30 keV) ions
throughout the heliosphere and beyond, is
possible with sensitive instrumentation to detect
the ENAs from charge exchange with interstellar
helium hydrogen
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Universities Involvement in Space
SciencesExcellence in ScienceInnovation in
TechnologyStudent Training Efficiency (Cheap)
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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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NASA Solar Probe mission (planned launch 2015
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