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| ACE | Contact: Tycho Von Rosenvinge, GSFC |
| Details | The Atmospheric Composition Explorer (ACE) makes in-situ particles and fields measurements as 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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| EIS | Contact: Len Culhane, MSSL |
| Details |
The EUV Imaging Spectrograph (EIS) provides monochromatic images and spectra of the transition region
and corona at high cadence using a slot. High spectral resolution images can be obtained by rastering with a slit. |
| SOT | Contact: Ted Tarbell, LMSAL |
| Details |
The Solar Optical Telescope (SOT) provides high resolution optical images. SOT also includes the Focal Plane Package (FPP) vector magnetograph and spectrograph. The vector magnetograph provides time series of photospheric vector magnetograms, Doppler velocity and photospheric intensity. The FPP spectrograph provides detailed Stokes line profiles. |
| XRT |
Contact: Ed De Luca, CFA |
| Details |
The X-Ray Telescope (XRT) provides high resolution images at a wide range of coronal temperatures, with both full disk and partial fields of view (for higher image cadence), and includes a flare flag. |
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| RHESSI | Contact: Brian Dennis, 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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| AIA | Contact: Alan Title, LMSAL |
| Details | The Atmospheric Imaging Assembly (AIA) images the solar atmosphere in multiple wavelengths to link changes in the surface to interior changes. Data includes images of the Sun in 10 wavelengths every 10 seconds. |
| EVE | Contact: Tom Woods, University of Colorado |
| Details |
The Extreme Ultraviolet Variablity Experiment (EVE) measures the solar
extreme-ultraviolet (EUV) irradiance with unprecedented spectral
resolution, temporal cadence, and precision. EVE measures the solar
extreme ultraviolet (EUV) spectral irradiance to understand variations
on the timescales which influence Earth's climate and near-Earth space. |
| HMI | Contact: Phil Scherrer, Stanford |
| Details |
The Helioseismic and Magnetic Imager (HMI) extends the capabilities of the
SOHO/MDI instrument with continual full-disk coverage at higher spatial
resolution and new vector magnetogram capabilities. |
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| SECCHI | Contact: Russ Howard, US Naval Research Laboratory |
| Details | The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) is comprised of four instruments: an extreme ultraviolet imager, two white-light coronagraphs and a heliospheric imager. These instruments study the 3-D evolution of CME's from birth at the Sun's surface through the corona and interplanetary medium to its eventual impact at Earth. |
| SWAVES | Contact: Michael L. Kaiser, CNRS, Paris |
| Details | The STEREO/WAVES (SWAVES) is an interplanetary radio burst tracker that traces the generation and evolution of traveling radio disturbances from the Sun to the orbit of Earth. |
| IMPACT | Contact: Janet Luhmann, University of California, Berkeley |
| Details | In-situ Measurements of Particles and CME Transients (IMPACT) samples the 3-D distribution and provides plasma characteristics of solar energetic particles and the local vector magnetic field. |
| PLASTIC | Contact: Toni Galvin, University of New Hampshire |
| Details | PLAsma and SupraThermal Ion Composition (PLASTIC) provides plasma characteristics of protons, alpha particles and heavy ions. This experiment provides diagnostic measurements of the form of mass and charge state composition of heavy ions and characterizes the CME plasma from ambient coronal plasma. |
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SWAP |
Contact:
Dan Seaton, Royal Observatory of Belgium |
| Details | SWAP is a single-band EUV coronal imager with a bandpass peak near 17.4 nm and angular resolution of 3.16 arcsec. SWAP's unique features include a relatively large field of view (54 arcmin) and the capability of offpointing flexibly in order to image extended or evolving off-limb features. In nominal mode, SWAP produces 1024x1024 images with an image cadence of roughly two minutes. |
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WIND |
Contact: Adam Szabo, GSFC |
| Details | The Wind spacecraft is a comprehensive solar wind monitor orbiting the Sun-Earth L1 Lagrange point making in-situ observations of the unperturbed solar wind. Wind instrumentation includes a fluxgate magnetometer, three different instruments to measure solar wind ions and also two for solar wind electrons, low and high energy particles, and radio and plasma waves. |