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Impulsive Energy Release in the Corona |
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Acceleration of Electrons, Protons, and Ions |
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Plasma Heating to Tens of Millions of degrees |
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Energy and Particle Transport and Dissipation |
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The Crab Nebula |
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Imaging
spectroscopy with 2” resolution |
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Gamma Ray Bursts and Cosmic Transient Sources |
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Detected
over a large fraction of the sky |
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High
resolution spectroscopy |
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Search
for cyclotron line features |
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Steady X-ray and gamma-ray sources (point and
diffuse) |
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Detect
by Earth occultation or through the rear grids |
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Obtain
high resolution spectra |
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Search
for line features |
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Hard X-ray Images |
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Angular
resolution as fine as 2 arcseconds |
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Temporal
resolution as fine as 10 ms |
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Energy
resolution of <1 keV to ~3 keV (FWHM) |
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High Resolution X-ray and Gamma-ray Spectra |
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~keV
energy resolution |
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To energies as high as 15 MeV |
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SOHO EUV images and spectra |
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Coronagraph images |
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Particle spectra and abundances |
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Yohkoh Images from both the soft and hard
X-ray telescopes |
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GOES Images from the Soft X-ray Imager |
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Wind & ACE Energetic particle spectra and
abundances, |
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low-frequency radio and energetic electrons |
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TRACE UV & XUV high resolution images |
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Ground-based Observatories |
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Radio and optical images and spectra |
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Magnetograms |
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Ha polarization |
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Hard X-Ray Imaging Spectroscopy |
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High Resolution Spectroscopy of Solar Gamma-Ray
Lines |
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Hard X-Ray and Gamma-Ray Imaging above 100 keV |
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Imaging of Narrow Gamma-Ray Lines |
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High Resolution X-ray and Gamma-Ray Spectra of
Cosmic Sources |
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Hard X-Ray Images of the Crab Nebula with 2-arcsecond Resolution |
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Microflares Tens of |
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thousands |
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Hard X-ray flares with crude imaging and
spectra >1000 |
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to >100 keV |
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Hard X-ray flares with >103 counts
s-1 detector-1 Hundreds |
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above 20 keV allowing spatial scales to be |
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followed on timescales of 0.1 s |
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Flares sufficiently intense to allow the
finest Tens |
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possible imaging spectroscopy |
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Flares with the detection of gamma-ray
lines Up to 100 |
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Flares with detailed gamma-ray line
spectroscopy Tens |
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and the location and extent of the source |
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determined to ~40 arcseconds |
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Energy Range 3 keV to 15 MeV |
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Energy Resolution (FWHM) <1 keV FWHM at 3
keV |
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increasing to 5 keV at 15 MeV |
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Angular Resolution 2 arcseconds to 100 keV |
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7 arcseconds to 400 keV |
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36 arcseconds to 15 MeV |
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Temporal Resolution Tens of ms for basic
image |
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2 s for detailed image |
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Field of View Full Sun |
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Effective Area - cm2 10-3
at 3 keV, 50 at 10 keV |
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(with attenuators out) 60 at 100 keV, 20 at 10 MeV |
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Numbers of flares ~1000 imaged to >100
keV. |
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~100 with spectroscopy to ~10 MeV |
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Instrument 9 germanium detectors (7.1-cm dia.
x 8.5 cm)
Cooled to 75 K with Sunpower cooler |
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Grid pitches from 34 microns to 2.75
mm |
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1.55-m grid separation |
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Solar Aspect System to <1
arcsecond |
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Roll Angle System to ~1 arcminute |
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Weight 130 kg |
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Power 125 watts |
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Telemetry 12 Gbits in 2 days |
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Spacecraft Spinning at 12 - 20 rpm |
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Pointing to within 0.1° of Sun
center |
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Launch Vehicle Pegasus XL from KSC |
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Orbit 38° inclination |
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600 km altitude, >3-year life |
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Launch Date March 2001 |
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Operations 2 years, 3 years highly desirable |
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Robert Lin University of California,
Berkeley PI |
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Gordon Hurford University of California,
Berkeley Imaging Scientist |
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Norman Madden LBNL, Berkeley Germanium
Detectors |
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Brian Dennis GSFC/682 Mission Scientist |
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Carol Crannell GSFC/682 Education &
Outreach |
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Gordon Holman GSFC/682 Flare Theory |
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Reuven Ramaty GSFC/661 Flare Theory |
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Tycho von Rosenvinge GSFC/661 ACE
Collaboration |
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Alex Zehnder Paul Scherrer Inst.
Switzerland Telescope design and fabrication |
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Frank van Beek Driebergen, The
Netherlands Grids and Imaging |
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Patricia Bornmann NOAA GOES Collaboration |
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Richard Canfield Montana State
University Ground-based Observations |
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Gordon Emslie Univ. of Alabama,
Huntsville Flare Theory |
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Hugh Hudson Solar Physics Research
Corp. Imaging |
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Arnold Benz Inst. of Astronomy, Zurich,
Switzerland Radio Observations |
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John Brown Univ. of Glasgow,
Scotland Flare Theory |
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Shinzo Enome NAO, Japan Radio Observations |
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Takeo Kosugi NAO, Japan Imaging |
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Nicole Vilmer Observatoire de Paris, Meudon,
France Data Analysis |
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University of California, Berkeley |
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David Smith Spectrometer Scientist |
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Jim McTiernan MOC/SOC Scientist |
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Isabel Hawkins Education & Outreach |
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Said Slassi-Sennou Spectrometer
Calibration |
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Andre Csillaghy Software |
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George Fisher Flare Theory |
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Chris Johns-Krull Modeling |
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GSFC |
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Richard Schwartz Data Analysis Software |
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Larry Orwig Grid Characterization |
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Dominic Zarro Complementary Data |
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University of Maryland |
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Ed Schmahl Imaging Software |
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Lockheed-Martin |
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Markus Aschwanden Timing Software |
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UC Berkeley Germanium detectors, cryostat,
& electronics |
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I & T |
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Ground station, MOC/SOC |
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Data Analysis |
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GSFC Grid characterization & testing |
|
Cryocooler |
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Data analysis, distribution, and archiving |
|
PSI (Switzerland) Telescope & aspect
system |
|
Thermo Electron Tecomet Finest grids (#1 - 4) |
|
van Beek (The Netherlands) Coarser grids (#5
- 9) & mounts |
|
Spectrum Astro Spacecraft |
|
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Science |
|
Dennis (682) Mission Scientist |
|
Holman (682), Ramaty (661) Solar flare
physics |
|
von Rosenvinge (661) ACE/HESSI
coordination |
|
Crannell (682) Education & Public
Outreach |
|
Imaging |
|
Clark (547) Imager metrology and testing |
|
Amato (544) Grid environmental testing |
|
Orwig (682) Optical & X-ray grid
characterization |
|
Uribe, Berg, Bilodeau (ITSS) |
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Spectrometer |
|
Boyle, Shirey (552) Cryostat design,
cooler evaluation |
|
Banks (OSC) Provide flight-qualified
Sunpower cooler |
|
Data Analysis |
|
Schwartz (Raytheon ITSS) Data analysis
software |
|
Tolbert (Raytheon ITSS) Graphical user
interface |
|
Schmahl (UMd) Image reconstruction |
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Zarro (EIT) Complementary data |
|
Gurman (682) Solar Data Analysis Center |
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