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85 results for “thermosphere”
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Wind Vectors Red
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Viewing Direction B Temperature
MIGHTI samples the O2 A band spectral region at five different wavelengths in order to both measure the shape of the band and to specify a background radiance that is subtracted from the signal. The wavelengths of the filter passbands are selected to maximize the sensitivity to lower thermospheric temperature variations. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. Two filter channels sample either end of the band to define a background (754.1 nm and 780.1 nm) and three more sample its shape (760.0 nm, 762.8 nm and 765.2 nm). Using three filters that sample the band shape allows the simultaneous retrieval of the atmospheric temperature and common shifts in the center wavelengths of the pass bands due to thermal drifts of the filters. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
Variations in Thermosphere during the 2018 SSW Event at Beijing and Wuhan
<p>SSW: temporal variations in stratospheric conditions prior to, during and after the SSW2018 from January 20 to March 21 (DOY 20 - DOY 80), 2018. First column: year; second volumn: DoY; third volumn: stratospheric temperature at 10h Pa at 60°N; fourth volumn: stratospheric temperature at 10h Pa between 60°N and 90°N; fifth volumn: velocity of zonal wind.</p> <p>average: average values between 1979 and 2017. first volumn: stratospheric temperature at 10h Pa at 60°N; second volumn: stratospheric temperature at 10h Pa between 60°N and 90°N; third volumn: velocity of zonal wind.</p> <p>F107andAp: temporal variations of F107 index and Ap index. First volumn: DoY; second volumn: local time; third volumn: F107 index; fourth volumn: Ap inex.</p> <p>Neden_Beijing/Wuhan:electron density at Beijing and Wuhan.</p> <p>date_Beijing/Wuhan: local time of elecrtron denisty.</p> <p>Tex_Beijing/Den_Beijing: retrieved Tex and corresponding neutral density at Beijing; DoY:20-80;LT:9:0.24:16;</p> <p>Tex_Wuhan/Den_Wuhan: retrieved Tex and corresponding neutral density at Wuhan; DoY:20-80;LT:9:0.24:16;</p> <p>Tex_Beijing_MSIS/Tex_Beijing_GCITEM: calculated Tex by empirical model NRLMSISE-00 and theoretical model GCITEM-IGGCAS at Beijing; DoY:20-80;LT:9:0.24:16;</p> <p>Tex_Wuhan_MSIS/Tex_Wuhan_GCITEM:calculated Tex by empirical model NRLMSISE-00 and theoretical model GCITEM-IGGCAS at Wuhan; DoY:20-80;LT:9:0.24:16;</p>
CASSIOPE GNSS-based thermospheric mass densities from 325 to 425 km at intervals of 25 km
<p>GNSS-based thermospheric mass densities from CAScade SmallSat and IOnospheric Polar Explorer (CASSIOPE). Densities from 325 to 425 km at intervals of 25 km. The fields are tab-delimited in the following order: Julian Date, latitude, longitude, altitude, and density estimates (Kg/m3) along orbit from CASSIOPE-GNSS, NRLMSISE-00, and JB2008.</p>
DE 2 Fabry-Perot Interferometer (FPI), Thermospheric Neutral Gas Density, Meridional Wind, and Temperature, 8-sec data
The Fabry-Perot Interferometer, FPI, was a High-Resolution Remote Sensing Instrument designed to measure the Thermospheric Temperature, Meridional Wind, and Density of the following Metastable Atoms: Atomic Oxygen, Singlet S and D, and the 2P State of Ionic Atomic Oxygen. The FPI performed a Wavelength Analysis on the Light detected from the Thermospheric Emission Features by spatially scanning the Interference Fringe Plane with a Multichannel Array Detector. The Wavelength Analysis characterized the Doppler Line Profile of the emitting Species. A Sequential Altitude Scan performed by a Commandable Horizon Scan Mirror provided a Cross-Sectional View of the Thermodynamic and Dynamic State of the Thermosphere below the DE 2 Orbit. The Information obtained from this Investigation was used to Study the Dynamic Response of the Thermosphere to the Energy Sources caused by Magnetospheric Electric Fields and the Absorption of Solar Ultraviolet Light in the Thermosphere. The Instrument was based on the Visible Airglow Experiment, VAE, used in the AE Program. The Addition of a Scanning Mirror, the Fabry-Perot Etalon, an Image Plane Detector, and a Calibration Lamp were the Principal Differences. Interference Filters isolated Lines at 5577, 6300, 7320, 5896, and 5200, in Angstroms. The FPI had a Field of View of 0.53°, Half-Cone Angle. More Details are found in P. B. Hays et al., Space Sci. Instrum., 5(4), 395, 1981. From February 16, 1982 to September 11, 1982 the DE Satellite was inverted and the FPI measured Galactic Emissions. NOTE: Animations of DE2-FPI Science Products have been created as Daily Summary Files. The Animations contain Binned Averages displayed as a Color Code against a Geographic Background. The Bin Sizes are 7.5° Latitude and 24.0° Longitude. The Longitude Bin corresponds to the approximate Separation of adjacent Orbits, assuming that DE2 completed 15 Orbits per Day. The Animations are divided by Day, 06-18 LST, and Night, 18-06 LST, where LST is Local Standard Time. All Summary File Information and Animations employ Spacecraft Orbital Attitude Data. Users should note 1, that the DE2-FPI Experiment acquired Airglow Spectra by imaging the Terrestrial Limb below and ahead of the Spacecraft at an approximate Tangent Altitude of 250 km, 2, All Airglow Spectra were acquired while the DE2 Spacecraft orbited in it's Normal Configuration, which corresponded to Calendar Months August to February in 1981 to 1982 and n 1982 to 1983; 3, The Orbital Inclination of DE2 was 90° implying that DE2-FPI always viewed Ahead along the Meridian; 4, And that DE2 flew in an Elliptical Orbit with Perigee of 305 km and Apogee of 1300 km at Launch ans the Attitude of DE2 for each FPI Measurement is included with each reduced Data Point permitting Users to determine the Tangent Latitude corresponding to the 250 km Terrestrial Airglow Limb. The three GIF Animations are: 1. FPI_brightness.gif, which documents the OI, 630.0 nm,, Column Brightness in Units of log10 Rayleighs. Note different Scales for Day and Night. 2. FPI_temperature.gif, which documents the Neutral Thermosphere Temperature in Units of °Kelvin. 3. FPI_wind.gif, which documents the Line of Sight Neutral Wind Component in Units of m/s. The Wind Direction is positive when the Wind blows away from the approaching Spacecraft.
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