2024-03-28T10:26:02.806Zhttps://cmr.earthdata.nasa.gov/opensearch/collections.atomCMRechodev@echo.nasa.govECHO dataset metadataSearch parameters: satellite => ACE boundingBox => geometry => placeName => startTime => endTime => uid => 12101https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614848-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) CRIS Level 2 DataThe Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer
(ACE) spacecraft is intended to be a major step in ascertaining the isotopic
composition of the Galactic Cosmic Rays and hence a major step in determining
their origin. The GCRs (Galactic Cosmic Rays) consist, by number, primarily of
hydrogen nuclei (~92%) and He nuclei (~7%). The heavier nuclei (1%) provide
most of the information about cosmic-ray origin through their elemental and
isotopic composition. The intensities of these heavy cosmic rays are very low
and progress in the past has been impeded by limited particle collection power,
particularly regarding individual isotopes. CRIS is designed to have far
greater collection power (~250 cm2*sr) than previous satellite instruments (<
10 cm2*sr) while still maintaining excellent isotopic resolution through Z=30
(Zinc) and beyond.
CRIS 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)
Currently, flux data are available for 24 elements, in units of
particles/(cm2*sr*sec*Mev/nucleon), in seven energy ranges. The energy ranges
are different for each element. The elements for which data are available are:
- B, C, N, O, F, Ne, Na, Mg, Al, Si, P, S, Cl, Ar, K, Ca, Sc, Ti, V, Cr,
Mn, Fe, Co, Ni
See:
http://www.srl.caltech.edu/ACE/ASC/level2/cris_l2desc.htmlC1214614848-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) CRIS Level 2 DataACE_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614862-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Electron, Proton, and Alpha Monitor (EPAM) Level 2 DataThe 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.htmlC1214614862-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Electron, Proton, and Alpha Monitor (EPAM) Level 2 DataACE_EPAM_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614850-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Magnetic Field Experiment (MAG) Level 2 DataThe Magnetic Field Experiment (MAG) consists of twin vector fluxgate
magnetometers controlled by a common CPU. The sensors are mounted on
booms extending 4.19 meters from the center of the spacecraft at
opposite sides along the +/-Y axes of the spacecraft. The instrument
returns 6 magnetic field vector measurements each second, divided
between the two sensors, with onboard snapshot and FFT buffers to
enhance the high-frequency resolution.
MAG 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 the magnetic
field data over the following time periods:
- 16 seconds
- 4 minutes
- hourly
- daily
- 27 days (1 Bartels rotation)
See:
http://www.srl.caltech.edu/ACE/ASC/level2/mag_l2desc.htmlC1214614850-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Magnetic Field Experiment (MAG) Level 2 DataACE_MAG_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214603832-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Particle Composition and Flux Browse DataThe 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.C1214603832-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Particle Composition and Flux Browse DataACE_PARTCLE_FLUXESNot providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEJHU/APL/SD/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614851-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Solar Energetic Particle Charge Analyser (SEPICA) Level 2 DataThe Solar Energetic Particle Charge Analyser (SEPICA) is used to
determine the charge state distribution of energetic particle
distributions. SEPICA is designed to measure the ionic charge state,
Q, the kinetic energy, E, and the nuclear charge, Z, of energetic ions
above 0.2 MeV/Nuc. This includes ions accelerated in solar flares as
well as in interplanetary space during energetic storm particle (ESP)
and co-rotating interaction region (CIR) events. For low mass numbers
SEPICA will also separate isotopes -- for example, 3He and 4He. During
solar quiet times, SEPICA should also be able to directly measure the
charge states of anomalous cosmic ray nuclei, including H, N, O, and
Ne, which are presumed to be singly-charged. With the capability to
differentiate the charge states of ions, the instrument will also be
able to separate neutral atoms (Q = 0) from ions. Thus it may be able
to identify energetic neutrals created through charge exchange.
SEPICA 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 energetic
particle fluxes over the following time periods:
- 120-second (H and He only)
- hourly
- (all elements) daily
- (all elements) 27 days (1 Bartels rotation) (all elements)
Currently, spin-averaged flux data are available for 8 elements, in
units of particles/(cm2*Sr*sec*MeV/nucleon), in a number of energy
ranges. The energy ranges are different for each element. The elements
for which data are available are:
- H, He, C, O, Ne, Mg, Si and Fe.
See:
http://www.srl.caltech.edu/ACE/ASC/level2/sepica_l2desc.htmlC1214614851-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Solar Energetic Particle Charge Analyser (SEPICA) Level 2 DataACE_SEPICA_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614863-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Solar Isotope Spectrometer (SIS) Level 2 DataThe 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.htmlC1214614863-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Solar Isotope Spectrometer (SIS) Level 2 DataACE_SIS_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614864-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM) Level 2 DataThe Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM) measures
the solar wind plasma electron and ion fluxes (rates of particle flow)
as functions of direction and energy. These data provide detailed
knowledge of the solar wind conditions and internal state every
minute. SWEPAM also provides real-time solar wind observations which
are continuously telemetered to the ground for space weather purposes.
Electron and ion measurements are made with separate sensors. The ion
sensor measures particle energies between about 0.26 and 36 KeV, and
the electron sensor's energy range is between 1 and 1350 eV. Both
sensors use electrostatic analyzers with fan-shaped
fields-of-view. The electrostatic analyzers measure the energy per
charge of each particle by bending their flight paths through the
system. The fields-of-view are swept across all solar wind directions
by the rotation of the spacecraft.
WEPAM 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:
- 64 seconds (ion data only)
- 128 seconds (electron data only)
- hourly
- (all data) daily
- (all data) 27 days (1 Bartels rotation) (all data)
SWEPAM level 2 data consists of the following data items:
- Ion data
o Proton Density (np in cm -3)
o Radial Component of the Proton Temperature (TP,rr in o Kelvin)
o Ratio of Alpha Density to proton Density (nHe/nP)
o Proton Speed (VP in km/s)
o Proton Velocity Vector in GSE coordinates (in km/s)
o Proton Velocity Vector in RTN coordinates (in km/s)
o Proton Velocity Vector in GSM coordinates (in km/s)
- Electron data
o Electron Temperature (in o Kelvin) (not yet available)
See:
http://www.srl.caltech.edu/ACE/ASC/level2/swepam_l2desc.htmlC1214614864-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM) Level 2 DataACE_SWEPAM_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614852-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Solar Wind Ion Composition Spectrometer (SWICS) and Solar Wind Ion Mass Spectrometer (SWIMS) Level 2 DataThe 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.htmlC1214614852-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Solar Wind Ion Composition Spectrometer (SWICS) and Solar Wind Ion Mass Spectrometer (SWIMS) Level 2 DataACE_SWICS_SWIMS_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214614832-SCIOPSCMRechodev@echo.nasa.govAdvanced Composition Explorer (ACE) Ultra Low Energy Isotope Spectrometer (ULEIS) Level 2 DataThe Ultra Low Energy Isotope Spectrometer (ULEIS) measures ion fluxes
over the charge range from H through Ni from about 20 keV/nucleon to
10 MeV/nucleon, thus covering both suprathermal and energetic particle
energy ranges. Exploratory measurements of ultra-heavy species (mass
range above Ni) will also be performed in a more limited energy range
near 0.5 MeV/nucleon. ULEIS will be studying the elemental and
isotopic composition of solar energetic particles, and the mechanisms
by which these particles are energized in the solar corona. ULEIS will
also investigate mechanisms by which supersonic interplanetary shock
waves energize ions.
ULEIS 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)
Currently, flux data are available for 7 species, in several energy
intervals for each species. Flux data are in units of particles/(cm2
Sr sec MeV/nucleon).
The species for which data are available are:
- H, 3He, 4He, C, O, Ne-S and Fe.
See:
http://www.srl.caltech.edu/ACE/ASC/level2/uleis_l2desc.htmlC1214614832-SCIOPS1997-08-25T00:00:00.000Z/Advanced Composition Explorer (ACE) Ultra Low Energy Isotope Spectrometer (ULEIS) Level 2 DataACE_ULEIS_LEVEL2Not providedSCIOPSCALTECH/SRL/ACECALTECH/SRL/ACEfalsefalsefalsefalsefalsefalsefalsefalse3.0830798https://cmr.earthdata.nasa.gov/opensearch/collections.atom?uid=C1214605489-SCIOPSCMRechodev@echo.nasa.govCoupling, Energetics, and Dynamics of Atmospheric Regions (CEDAR) Database at NCAR/HAOThe 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_PageC1214605489-SCIOPS1966-01-01T00:00:00.000Z/Coupling, Energetics, and Dynamics of Atmospheric Regions (CEDAR) Database at NCAR/HAOCEDAR_NCAR_HAONot providedSCIOPSUCAR/NCAR/HAO/CEDARUCAR/NCAR/HAO/CEDARCARTESIAN-90 -180 90 180falsefalsefalsefalsefalsefalsefalsefalse0.85800005org.geoss.geoss_data-coretrue