Max Millennium Program

Collaborating Space Based Observatories

  • ACE
  • HXRS
  • SOHO

    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,
    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. 
    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.
    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
    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.
    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  
    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]. 
    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.