2.0.1 spase://vspo/numericalData/P_ACE_HDR_SEPICA_2M ACE SEPICA L2 2-min H and He flux data 2007-06-01T00:00:00 ACE SEPICA L2 2-min H and He flux data, by charge states, at ASC spase://SMWG/Person/Eberhard.S.Moebius PrincipalInvestigator spase://SMWG/Repository/ACE_SC Online Open ACE Science Center (ASC) http://www.srl.caltech.edu/ACE/ASC/level2/lvl2DATA_SEPICA.html in HDF via ftp from ASC ftp://mussel.srl.caltech.edu/pub/ace/level2/sepica/ Text CALIBRATED spase://SMWG/Instrument/ACE/SEPICA EnergeticParticles IonComposition 1997-10-07T00:00:00 -P14D Data are presently ~2 weeks delayed PT120S Heliosphere.NearEarth spase://SMWG/Observatory/ACE ACE Advanced Composition Explorer 1997-045A Explorer 71 2009-05-20T20:00:12Z The objective of the Advanced Composition Explorer (ACE) is to collect observations of particles of solar, interplanetary, interstellar, and galactic origins, spanning the energy range from that of KeV solar wind ions to galactic cosmic ray nuclei up to 600 MeV/nucleon. Definitive studies will be made of the abundances of essentially all isotopes from H to Zn (Z = 1-30), with exploratory isotope studies extending to Zr (Z = 40). The ACE payload includes six high resolution spectrometers, each designed to provide the optimum charge, mass, or charge-state resolution in its particular energy range. Each spectrometer has a geometry factor optimized for the expected flux levels, so as to provide a collecting power greater by a factor of 10-1000 times that of previous or planned experiments. The payload also includes three additional instruments of standard design to monitor energetic electrons, H and He ions, and a magnetometer. The ACE spacecraft is based on the design of the Charge Composition Explorer, built at JHU/APL for the Active Magnetospheric Particle Tracer Explorer (AMPTE) program. The spacecraft spin axis is pointed towards the Sun to within +/- 20 degrees, and it occupies a halo orbit about the L1 Earth-Sun libration point. Powered by solar cells, the spacecraft has a design life of at least five years, and it returns data in daily tape recorder dumps, received through NASA JPL's Deep Space Network and initially processed at NASA-GSFC. The average data telemetry rate is 6.7 Kbs. spase://SMWG/Person/Edward.C.Stone.Jr PrincipalInvestigator ACE Home Page http://www.srl.caltech.edu/ACE/ ACE mission home page at Caltech with data download NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1997-045A Information about the ACE mission spase://vspo/observatory/2 Heliosphere.NearEarth Heliosphere.Inner spase://SMWG/Instrument/ACE/SEPICA Solar Energetic Particle Ionic Charge Analyzer (SEPICA) SEPICA 2009-05-20T21:10:13Z The Solar Energetic Particle Ionic Charge Analyzer (SEPICA) is designed to measure ionic charge state, kinetic energy, and nuclear charge of energetic ions at energies above 0.2 MeV/nucleon. Principal science goals include measurement of such ions from solar flares, coronal and interplanetary shocks, co-rotating interaction regions, and the solar wind termination shock, the latter being the probable source of the anomalous cosmic ray component. The SEPICA sensors combine electrostatic deflection of incoming ions in a collimator analyzer with a differential energy loss (dE/dx) vs. residual energy telescope. Energetic ions entering the multi-split collimator, which focuses the ions on a line in the detector plane, are electrostatically deflected between a set of electrode plates at voltage potentials up to 30 kV. The amount of deflection, inversely proportional to energy per charge, is measured in a multi-wire thin-window proportional counter. This counter is also used to measure the dE/dx of the ion. Residual energy of the ion is then determined in a solid-state detector behind the proportional counter. A CsI anticoincidence scintillator behind the solid state detector is used to supress background events from penetrating high energy particles. The SEPICA instrument array consists of three pairs of telescopes with collimators, electrostatic deflection electrodes, proportional counters, and solid state detectors. Each pair shares a high-voltage deflection electrode. Two of the pairs have collimators with larger geometric factor for higher sensitivity to smaller solar energetic particle (SEP) events. The third pair uses a fine collimator to reduce the geometric factor for improved charge state resolution. The field of view (FOV) of each telescope is 24 deg. x 50 deg. with 0.36 sq.cm.-sr for the large geometric factor sensors and 0.06 sq.cm.sr for those with the fine collimator. Charge resolution is about 10 percent with the fine collimator. The SEPICA data rate of 604 bps includes readout of 46 bits/events for 12 pulse height analysis (PHA) events/s, sectored (8) counting rates for He and Z>2 ions at 60-sec resolution, 64 PHA matrix rates at 300-sec resolution, and various housekeeping data. The SEPICA experiment manager is Dr. Eberhard Mobius of the University of New Hampshire. spase://SMWG/Person/Eberhard.S.Moebius PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1997-045A&ex=4 Information about the Solar Energetic Particle Ionic Charge Analyzer (SEPICA) experiment on the ACE mission. ElectrostaticAnalyser Solar Energetic Particle Ionic Charge Analyzer (SEPICA) on ACE spase://SMWG/Observatory/ACE spase://SMWG/Repository/ACE_SC SRL ACE Science Center ASC 2008-06-18T06:07:48Z ACE Science Center Please acknowledge the ACE instrument teams and the ACE Science Center in publications and presentations that use these data spase://SMWG/Person/Andrew.J.Davis PrincipalInvestigator GeneralContact ACE Science Center http://www.srl.caltech.edu/ACE/ASC spase://SMWG/Person/Andrew.J.Davis Dr. Andrew J. Davis California Institute of Technology spase://SMWG/Person/Eberhard.S.Moebius Dr. Eberhard S. Moebius University of New Hampshire spase://SMWG/Person/Edward.C.Stone.Jr 2001-04-02T00:00:00Z Prof. Edward C. Stone, Jr. California Institute of Technology ecs@srl.caltech.edu +1-626-395-8321