The Electron, Proton, and Alpha Monitor (EPAM) is composed of five telescope apertures of three different types. Two Low Energy Foil Spectrometers (LEFS) measure the flux and direction of electrons above 30 keV (geometry factor = 0.397 cm2*sr), two Low Energy Magnetic Spectrometers (LEMS) measure the flux and direction of ions greater than 50 keV (geometry factor = 0.48 cm2*sr), and the Composition Aperture (CA) measures the elemental composition of the ions (geometry factor = 0.24 cm2*sr). The telescopes use the spin of the spacecraft to sweep the full sky. Solid-state detectors are used to measure the energy and composition of the incoming particles. EPAM Level 2 data is organized into 27-day time periods (Bartels Rotations - roughly one solar rotation period). For each Bartels Rotation, the Level 2 data contains time averages of energetic charged particle fluxes over the following time periods: - hourly - daily - 27 days (1 Bartels rotation) The DE30 detector, (Deflected Electrons), measures electrons at 30 degrees from the spacecraft spin axis. Electrons entering the LEMS30 detector are swept out by a rare-earth magnet and are deflected into the B detector. The 4 DE channels are pure electron channels. The geometrical factor for the DE30 channels is 0.14 (cm2*sr). The CA60 telescope, (Composition Aperture) measures ion composition. It's look-direction is oriented 60 degrees from the spacecraft spin-axis. The CA telescope is capable of determining ion composition using a dE X E detection scheme. Although the principal responsibility of EPAM is to monitor electrons, protons, and alphas, the CA provides an unambiguous determination of ion composition, unlike the LEMS detectors. The CA60 telescope is comprised of three solid state detectors, a thin, ~5 micron epitaxial silicon detector referred to as the D detector, and two thick (200 micron) totally depleted surface barrier silicon detectors known as C and B. The B detector, as measures deflected electrons from the LEMS30 head, but also acts as the anti-coincidence detector for the CA. The CA system uses log amplifiers to extend the dynamic range of the detector. These amplifiers are extremely temperature sensitive, and therefore are thermally regulated with heaters to maintain calibration. The logic used in the CA depends on slanted discriminators to define each species group. The eight Ca rate channels, denoted by the symbols W1 - W8, count all particles in a given energy/nucleon range. Multiple species may therefore be associated with a single Ca rate channel. As a result, a species group is identified by the dominant species in that group. See: http://www.srl.caltech.edu/ACE/ASC/level2/epam_l2desc.html

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• ACE_EPAM_LEVEL2

SCIOPS Short Name: ACE_EPAM_LEVEL2 Version ID: Not provided Unique ID: C1214614862-SCIOPS

The Advanced Composition Explorer (ACE) is an Explorer mission that is being managed by the Office of Space Science Mission and Payload Development Division of the National Aeronautics and Space Administration (NASA). The primary purpose of ACE is to determine and compare the isotopic and elemental composition of several distinct samples of matter, including the solar corona, the interplanetary medium, the local interstellar medium, and Galactic matter. The ACE spacecraft measures the flux of charged particles from solar wind energies (300 km/sec) up through galactic cosmic rays (500 MeV/nucleon) and the interplanetary magnetic field upstream of earth. The ACE data includes energetic particles from solar wind cosmic ray energies. In addition, this data set covers both atomic and isotopic composition data for most energy ranges. This pace data is at L1 (approx. 1.5 million km upstream along earth-sun line). ACE browse data are designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data are automatically generated from the spacecraft data stream using simple algorithms provided by the instrument investigators. They are not routinely checked for accuracy and are subject to revision. Use these data at your own risk, and consult with the appropriate instrument investigators about citing them. Browse parameters are a subset of measurements by the ACE instruments which are created at the Science Center during level one processing. They are delivered to the public domain as soon as possible. Their purpose is to allow monitoring of the solar wind and large-scale particle and magnetic field behavior, and selection of interesting time periods for more intensive study. Interesting time periods might include solar energetic particle events, or the passage of an interplanetary shock. An additional use of the browse parameters is to investigate relationships between the data from the various ACE instruments, and between ACE data and data from other sources. The browse parameters include unsectored fluxes of ions at many different energies and electrons at a few energies. They also include the interplanetary magnetic field, and solar wind parameters such as proton speed and temperature. They therefore furnish a very abbreviated description of what is being observed by the ACE instruments, without the relatively high cost of storing and analyzing all the level one data. Eventually they may be supplemented with event data from the particle detectors, but experience with the flight data is a prerequisite for delivering useful products of that type. See: http://www.srl.caltech.edu/ACE/ASC/browse/browse_info.html for more information.

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• ACE_PARTCLE_FLUXES

SCIOPS Short Name: ACE_PARTCLE_FLUXES Version ID: Not provided Unique ID: C1214603832-SCIOPS

The Solar Isotope Spectrometer (SIS) is designed to provide high resolution measurements of the isotopic composition of energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to ~100 MeV/nucleon. During large solar events, when particle fluxes can increase over quiet-time values by factors of up to 10000, SIS measures the isotopic composition of the solar corona, while during solar quiet times SIS measures the isotopes of low-energy Galactic cosmic rays and the composition of the anomalous cosmic rays which are thought to originate in the nearby interstellar medium. The solar energetic particle measurements are useful to further our understanding of the Sun, while also providing a baseline for comparison with the Galactic cosmic ray measurements carried out by CRIS. SIS has a geometry factor of ~40 cm2--sr, which is significantly larger than previous satellite solar particle isotope spectrometers. It is also designed to provide excellent mass resolution during the extremely high particle flux conditions which occur during large solar particle events. SIS level 2 data is organized into 27-day time periods (Bartels Rotations - roughly one solar rotation period). For each Bartels Rotation, the level 2 data contains time averages of energetic charged particle fluxes over the following time periods: - 256 seconds - hourly - daily - 27 days (1 Bartels rotation) Currently, flux data are available for 8 elements, in units of particles/(cm2 Sr sec MeV/nucleon), in eight energy ranges. The energy ranges are different for each element. The elements for which data are available are: - He, C, N, O, Ne, Mg, Si, S, and Fe. See: http://www.srl.caltech.edu/ACE/ASC/level2/sis_l2desc.html

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• ACE_SIS_LEVEL2

SCIOPS Short Name: ACE_SIS_LEVEL2 Version ID: Not provided Unique ID: C1214614863-SCIOPS

The Solar Wind Ion Composition Spectrometer (SWICS) and the Solar Wind Ion Mass Spectrometer (SWIMS) on ACE are instruments optimized for measurements of the chemical and isotopic composition of solar and interstellar matter. SWICS determines uniquely the chemical and ionic-charge composition of the solar wind, the temperatures and mean speeds of all major solar-wind ions, from H through Fe, at all solar wind speeds above 300 km/s (protons) and 170 km/s (Fe+16), and resolves H and He isotopes of both solar and interstellar sources. SWICS will measure the distribution functions of both the interstellar cloud and dust cloud pickup ions up to energies of 100 keV/e. SWIMS will measure the chemical and isotopic and charge state composition of the solar wind for every element between He and Ni. Each of the two instruments uses electrostatic analysis followed by a time-of-flight and, as required, an energy measurement. The observations made with SWICS and SWIMS will make valuable contributions to the ISTP objectives by providing information regarding the composition and energy distribution of matter entering the magnetosphere. SWICS level 2 data is organized into 27-day time periods (Bartels Rotations - roughly one solar rotation period). For each Bartels Rotation, the level 2 data contains time averages of solar wind parameters over the following time periods: - hourly - daily - 27 days (1 Bartels rotation) SWICS level 2 data consists of the following solar wind data items: - Bulk and Thermal ion Speeds (km/s) => H+, He+2, O+6, Mg+10, and Fe+11 - Ratio of Elements => 4He+2/O, 20Ne+8/O, 24Mg+10/O, and 56Fe+(7 to 12)/O - Ratio of Charge States of the Same Element => C+5/C+6, O+7/O+6, and Fe+11/Fe+9 - Isotope ratios => 3He/4He, 22Ne/20Ne, 24Mg/26Mg See: http://www.srl.caltech.edu/ACE/ASC/level2/swics_swims_l2desc.html

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• ACE_SWICS_SWIMS_LEVEL2

SCIOPS Short Name: ACE_SWICS_SWIMS_LEVEL2 Version ID: Not provided Unique ID: C1214614852-SCIOPS

The Coupling, Energetics, and Dynamics of Atmospheric regions (CEDAR) is a program sponsored by the National Science Foundation (NSF) designed to enhance the capability of ground-based instruments to measure the upper atmosphere and to coordinate instrument and model data for the benefit of the scientific community. The CEDAR Data Base (formally the Incoherent Scatter Radar Data Base) is a cooperative project between the National Center for Atmospheric Research (NCAR) and several institutions that provide upper atmosphere data and model output for community use. The CEDAR Data Base contains: documentation, catalogue information, geophysical indices, summary plots, analysis software, and computer models. A catalogue is produced every year and is available on the WWW at: http://cedarweb.hao.ucar.edu/wiki/index.php/Main_Page CEDAR instruments are located throughout the world. Only selected data from each instrument is available in the CEDAR Data Base. The on-line CEDAR Data Base contains information to contact investigators for additional data not found in the Data Base. The CEDAR Data Base currently contains approximately 10GB of data. A complete inventory of data and data availability is obtainable from the following: http://cedarweb.hao.ucar.edu/wiki/index.php/Main_Page The CEDAR Data Base consists of the following: Geophysical Indices. Includes Dst, Kp, ap, Ap, solar 10.7 cm flux, sunspot number, AE, and IMF parameters. Large Model Output. Includes model output from the Assimilative Mapping of Ionospheric Electrodynamics (AMIE), Thermosphere Ionosphere General Circulation Model (TIGCM), and Global-Scale Wave Model (GSWM). Incoherent Scatter Radar. This is the primary data in the CEDAR Data Base. Includes ionospheric electron densities, ion velocities, and electron and ion temperatures. Ionospheric Doppler Radars. HF ionospheric doppler radars are organized into a collection of radars called SuperDARN (Super Dual Auroral Radar Network). Eleven radars have data in the CEDAR Data Base. Basic parameters include line-of-sight plasma irregularity and velocity spread. Digisondes. Consists of ion drift data from the Qaanaaq Digisonde. Fabry-Perot Interferometers. Basic parameters from FPI are brightness, neutral temperature, and line-of-sight neutral winds. IR Michelson Interferometers. Data include neutral temperatures derived from nightglow hydroxyl (OH). Lidar. Basic Lidar parameters are photocounts, relative neutral number density, and sodium or iron density. Middle Atmosphere Radars. Data are from MST radars, MF radars, LF radars, meteor wind radars and ST radars. There is only limited data in the CEDAR Data Base. Parameters include line-of-sight neutral winds and turbulence. Airglow Imagers and All-Sky Cameras. Data includes brightness data from imagers. None of the imager data are in digital form. Some airglow data is on video tape. Models. Consists of both theoretical models and empirical models. Source code is available from the CEDAR Data Base. Model output consists of geomagnetic field data, electron densities, electric fields, interpolations and models of NOAA and DMSP satellite data, wind models, ionospheric parameters, and other data. The CEDAR Data Base is accessible through the WWW and ftp, but users must have a valid access form, available from the WWW or ftp (see Access and Use constraints) or contact Barbara Emery (emery@ucar.edu ). See the WWW site for additional information on accessing the data and Rules of the Road procedures. http://cedarweb.hao.ucar.edu/wiki/index.php/Main_Page

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• CEDAR_NCAR_HAO

SCIOPS Short Name: CEDAR_NCAR_HAO Version ID: Not provided Unique ID: C1214605489-SCIOPS