Hourly-averaged near-Earth solar wind magnetic field and plasma, etc. The web services consists of OMNI data (spacecraft-interspersed, near-Earth solar wind data); spacecraft-specific data sets (near 1 AU, including near-Earth) including ACE, Geotail, IMP-8, IMP6&7, Wind, Explorer 33&35, Genesis, ISEE 3, Prognoz, SOHO, GOES, and Moon. Data also includes deep space data including COHOWeb-formatted hourly solar wind field and plasma, Pioneer, Ulysses, Voyager, Cassini, Helios, Mariner, and STEREO; and Interfaces for comparing multi-source data. The Space Physics Data Facility (SPDF) is the archive of non-solar data for the Heliospheric Science Division (HSD) at NASA's Goddard Space Flight Center.

국립중앙과학관 홈페이지에 있는 과학학습콘텐츠의 전시보유품 파일 목록입니다.데이터 항목명: 고유 아이디, 전시품 아이디, 이름, 저장된 파일명, 저장경로, 전시타입, 파일설명, 공개여부, 등록자 아이디※ 대전광역시 유성구 대덕대로 481(국립중앙과학관)

Heliocentric trajectories for Mars Science Laboratory in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinates The original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth. The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch", which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage: +---------------------------------------------------------------------+ Method Name FPA Longitude Definition --------------------------------------------------------------------- B1950.0 the actual FPA at 22:09 UT on December 31, 1949 J2000.0 the smoothed FPA at 12:00 UT on January 1, 2000 True of Date the actual FPA at 00:00 UT on the date of interest Mean of Date the smoothed FPA at 00:00 UT on the date of interest +---------------------------------------------------------------------+ The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method. More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.

The NSSDC Coordinated Heliospheric Observations Web, COHOWeb, hourly and daily Solar-Terrestrial Relations Observatory-A, STEREO-B, data were made by using high resolution data from from CDAWeb. The STEREO-A COHO file include data derived from the STEREO-A In-Situ Measurements of Particles and CME Transients, IMPACT, Fluxgate Magnetometer data, Thermal Plasma Moments: Solar Wind Proton and Ion Densities, Speeds, Velocity Vector Flow Angles, and Temperatures from the STEREO-A Plasma and Supra-Thermal Ion Composition, PLASTIC, Instrument, and Energetic Particle Fluxes from the STEREO-A IMPACT Solar Energetic Particle, SEP, Instrument Suite including the Low Energy Telescope, LET, High Energy Telescope, HET, and Suprathermal Ion Telescope, SIT. COHOWeb's magnetic field hourly averages were created at GSFC/SPDF by averaging over the six 10-min averages falling within each hour. Hourly plasma parameter data were obtained from UNH via http://fiji.sr.unh.edu/1dmax_ascii/.

The NSSDC Coordinated Heliospheric Observations Web, COHOWeb, hourly and daily Solar-Terrestrial Relations Observatory-A, STEREO-B, data were made by using high resolution data from from CDAWeb. The STEREO-A COHO file include data derived from the STEREO-A In-Situ Measurements of Particles and CME Transients, IMPACT, Fluxgate Magnetometer data, Thermal Plasma Moments: Solar Wind Proton and Ion Densities, Speeds, Velocity Vector Flow Angles, and Temperatures from the STEREO-A Plasma and Supra-Thermal Ion Composition, PLASTIC, Instrument, and Energetic Particle Fluxes from the STEREO-A IMPACT Solar Energetic Particle, SEP, Instrument Suite including the Low Energy Telescope, LET, High Energy Telescope, HET, and Suprathermal Ion Telescope, SIT. COHOWeb's magnetic field hourly averages were created at GSFC/SPDF by averaging over the six 10-min averages falling within each hour. Hourly plasma parameter data were obtained from UNH via http://fiji.sr.unh.edu/1dmax_ascii/.

The TIROS/NOAA satellite series, also known as POES, is designed to meet the National Oceanic and Atmospheric Administration's need for operational, remote sensing products for numerical weather and space environment forecasts. The TIROS designation represents the experimental classification of a new instrument configuration while NOAA represents the operational classification. For January 1979 through present, the National Centers for Environmental Information (formerly National Geophysical Data Center) archive data from the POES Space Environment Monitor instrument. Subcomponents of the SEM include: HEPAD (High Energy Proton and Alpha Detector), MEPAD (Medium Energy) and TED (Total Energy) data from TIROS and NOAA satellites. The satellites are in sun-synchronous orbits at 850 kilometers altitude, an orbital period of 102 minutes and an inclination of 99 degrees. The orbital plane is tilted toward the sun in the Northern Hemisphere. Usually, two satellites are operational at all times.NOAA's Polar Orbiting Environmental Satellites (POES) (formerly known as TIROS for Television and InfraRed Observation Satellite) carry a suite of instruments that detect and monitor the influx of energetic ions and electrons into the atmosphere and the particle radiation environment at the altitude of the satellite. Both phenomena vary as a result of solar and geomagnetic activity. Beginning with the NOAA-15 satellite, an upgraded version of the Space Environment Monitor (SEM-2) is being flown. A number of SEM-2 instruments have been procured and it is anticipated that the SEM-2 instruments will be included on the NOAA/POES satellites until superceded by the NPOESS satellite program sometime after 2010.Because the SEM-2 instruments differ significantly from the earlier SEM-1, there has been a complete revision to the data processing and archiving process. A number of improvements have also been included. Among these are incorporating up-to-date satellite orbit information and magnetic field models in the calculation of various magnetic coordinates, and improved data quality control. The Total Energy Detector (TED) is designed to measure the energy flux carried by auroral particles, both positively charged ions (assumed here to be protons) and electrons, into the polar atmosphere. The magnitude and spatial extent of this energy flux are good measures of both the level of auroral activity and the atmospheric response to that energy input. The Medium Energy Proton and Electron Detector (MEPED) includes a set of solid-state energetic particle detectors that monitor the intensities of protons and electrons over a range extending from 30 keV to more than 200 MeV. Particles having those energies include the radiation belt (Van Allen belt) populations, the particles in energetic solar particle events (solar proton events), and the low energy portion of the galactic cosmic ray population. Enhanced fluxes of these particles entering the atmosphere can produce significant and widespread degradation in short-wave radio propagation; in extreme cases even radio blackouts. The energetic particles also contribute to astronaut radiation exposure, especially on high inclination orbit missions during energetic solar particle events.

Advanced Composition Explorer (ACE) observes particles of solar, interplanetary, interstellar, and galactic origins.

Collection includes a variety of space weather datasets from the National Oceanic and Atmospheric Administration and from the World Data Service for Geophysics, Boulder.

'The ISS SERVIR Environmental Research and Visualization System (ISERV) acquired images of the Earth\'s surface from the International Space Station (ISS). The goal was to improve automatic image capturing and data transfer. ISERV\'s main component was the optical assembly which consisted of a 9.25 inch Schmidt-Cassegrain telescope, a focal reducer (field of view enlarger), a digital single lens reflex camera, and a high precision focusing mechanism. A motorized 2-axis pointing mount allowed pointing at targets approximately 23 degrees from nadir in both along- and across-track directions. '