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ACE | Contact: Tycho Von Rosenvinge, GSFC |
Details | ACE orbits the L1 libration point in an elliptical orbit with a semi-major axis of approximately 200,000 km. ACE instruments include: CRIS Cosmic Ray Isotope Spectrometer, EPAM Electon, Proton, and Alpha Monitor, MAG Magnetometer, SEPICA Solar Energetic Particle Ionic Charge Analyzer, SIS Solar Isotope Spectrometer, SWEPAM Solar Wind Electon, Proton, and Alpha Monitor, SWICS Solar Wind Ionic Charge Spectrometer, SWIMS Solar Wind Ion Mass Spectrometer, & ULEIS Ultra Low Energy Isotope Spectrometer, |
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SXT | Contact: Doug Biesecker, NOAA |
Details | 3-80 Angstrom Soft X-ray images. Full disk images with pixel size 5" in a 512 x 512 array and an image cadence of 1/minute. |
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RHESSI | Contact: Dominic Zarro, GSFC |
Details | Angular Resolution: 2 arcseconds to 100 keV, 7 arcseconds to 400 keV, 36 arcseconds above 1 MeV. Angular Coverage: sources of size ~2 arcseconds to ~180 arcseconds can be imaged anywhere within the ~1-degree RHESSI field of view centered within 0.2 degrees of Sun center. Temporal Resolution: Tens of milliseconds for a basic image. 2 seconds (half a rotation of the spacecraft) for a detailed image. Spectral Resolution: 0.5 keV (FWHM) to 30 keV, increasing to ~3 keV at 1 MeV, ~5 keV at 20 MeV. Aspect information: direction to Sun-center to better than 1.5", roll angle to better than 3'. Direct questions about RHESSI status and operations to the RHESSI Tohban. |
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HXRS | Contact: Frantisek Farnik, Ondrejov or Howard Garcia, NOAA or Alan Kiplinger, CU. |
Details | This full-disk hard X-ray spectrometer covers the energy range 12.6 to 250 keV, divided into eight, approximately equal logarithmic energy bands. Observations have a 1 second time resolution in monitor mode and 200 ms in flare mode. The satellite experiences 35 minutes of earth occultation and four passages through the radiation belts on each orbit, yielding an approximate 40% observing efficiency. HXRS observations of selected >M1 importance flares, relatively free of particle contamination, are available at http://www.asu.cas.cz/HXRS/. |
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RF-15I | Contact: Marek Siarkowski, SRC, PAS |
Details | Full disk X-ray photometry from the INTERBALL RF-15I instrument. Energy range about 1 kev and 10-15-30-60-120-240 keV with time resolution 0.125 - 8 sec. |
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CDS | Contact: Andrzej Fludra, GSFC |
Details | Continuous tracking of the target active region. Imaging in FeXIX, FeXVI, MgX, OV and He1 at 10 minute cadence. The field of view will be 3 by 3 arc-minutes at a resolution of 4arc-seconds. |
EIT | Contact: Joe Gurman, GSFC |
Details | Normal synoptic images (full sun, full resolution 304A, 171A, 284A, and 195A every 6 hrs) and 195A CME Watch (full sun, 12 minute cadence, full resolution when SUMER not observing, half resolution when SUMER is observing). |
LASCO | Contact: Simon Plunkett, NRL |
Details | C2 and C3 synoptics: Nearly regular cadence of C2 and C3 images obtained often enough to allow measurement of the acceleration of CME's moving at plane-of-the-sky speeds of less than ~ 1000 km/s. (see also http://lasco-www.nrl.navy.mil/lasco.html |
SUMER | Contact: Davina Innes, MPI |
Details | Limb targets only. Sit and stare spectra along the 300 arcsec slit, positioned between 50-100 arcsec off the limb. The line selection will include at least one hot flare line (FeXXI, FeXIX, FeXVIII, FeXVII), one million degree line (CaXIV, FeXII, CaX) and a cold line (SiIII, CIII, HI). Time cadence between 50-300s. |
MDI | Contact: Rock Bush, Stanford |
Details | Full disk magnetograms, continuum imaging and Dopplergrams at a maximum possible time resolution allowable, dictated by DSN contact and present MDI observing mode. When DNS contacts are not optimal, this means magnetograms only, with 96 minute cadence. |
UVCS | Contact: John Raymond, CFA |
Details | For target regions close to the limb, UVCS can perform a CME watch. Default parameters are slit height = 2.3 solar radii, 120 second integrations, 21 arc-second spatial binning, and coverage of Ly alpha, Ly beta, and lines of O VI, Si XII, C III and [Fe XVIII]. |
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TRACE | Contact: Harry Warren, CFA |
Details | 1600 A (for flare flag) and one EUV line (171 or 195 A) image sequences. The flare flag triggers a high cadence (approximately 10 second) flare-mode image sequence in one EUV line (either 171 or 195) with occasional context images in the other TRACE bands. |