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85 results for “thermosphere”
Water "Pump" in the Atmosphere of Mars: Modeling Vertical Transport to the Thermosphere
<p>Recent studies link the observed hydrogen escape in the Martian thermosphere to the water of lower atmospheric origin. However, the cold mesosphere hinders penetration of vapor into the upper atmosphere. We present results of simulations with the Max Planck Institute general circulation model (MPI-MGCM) implementing a state-of-the-art hydrological cycle scheme. The simulations reveal a seasonal water ``pump” mechanism responsible for the upward transport of vapor. It takes place in high latitudes of the southern hemisphere at perihelion, when the upward branch of the meridional circulation is particular strong. A combination of the mean vertical flux with variations induced by solar tides facilitates penetration of water across the “bottleneck” at approximately 60 km. The meridional circulation then transports water across the globe to the northern hemisphere. Since the intensity of the meridional cell is tightly controlled by airborne dust, the water abundance in the thermosphere strongly increases during dust storms.</p>
Thermospheric neutral wind and temperature over Cachoeira Paulista
<p>The data sets are observations of thermospheric neutral winds and temperatures which can be used to study the dynamics of low latitude ionosphere in Brazil. The data have been organized by Dr Jonas R. Souza (jonas.souza@inpe.br) from National Institute for Space Research - INPE.</p>
HIWIND Observation of Summer Season Polar Cap Thermospheric Winds
The dataset includes 1) balloon-borne instrument HIWIND observed thermospheric winds in the polar cap, and 2) TIEGCM simulation of the polar cap electron density and thermospheric winds with normal soft electron precipitation and more soft electron precipitation. The dataset will be used in a publication with the same title.
Hemispheric Asymmetry of the Annual and Semiannual Variation of Thermospheric Composition
This dataset includes O, O2, and N2 number densities in the altitude region from 110.1 km to 667.5 km derived from TIMED/GUVI limb observation and the corresponding WACCM-X simulated ones. These data are daily average values in five latitude bins from 50 degree south to 50 degree north with a bin size of 20 degrees, and number of data points and observing local times for the data in the latitude bins. They are used to make Figures 1-10 in the paper with the title the same as the title for this dataset.
Solar wind power likely governs Uranus' thermosphere temperature
<p>Derived data shown in Figure 1 for the publication in Geophysical Research Letters.</p>
Equatorial nighttime thermospheric zonal wind jet response to the temporal oscillation of solar wind
<p>The simulation data processed in Matlab</p>
Empirical Model of Thermospheric NO cooling Based on SABER observation
<p>This thermospheric NO cooling model is deverived from SABER observation within 100-280 km altitude. The vertical structure is derived from PCA method and the horizontal distribution is reconstruced by the consequence nonlinear regression technic.</p>
Thermospheric neutral wind and temperature over Cachoeira Paulista
<p>The datasets are observations of thermospheric neutral winds and temperatures recorded by a Fabry-Perot interferometer. These data can be used to study the dynamics of the low-latitude ionosphere in Brazil. The data were organized by Dr. Jonas R. Souza (jonas.souza@inpe.br) from the National Institute for Space Research - INPE.</p>
Investigation of anomalous transport in the lower thermosphere Project
<p align="LEFT"> &nbsp;</p> <p> <font size="3">Near-simultaneously deployed chemical tracer trails over an extended horizontal range will be used to obtain measurements of the turbulent structure function and (the pair) relative velocity distribution over a range of spatial scales covering a full decade. </font></p> <p> <font size="3">Trimethyl aluminum trails (TMA) released in the mesosphere and lower thermosphere have been used to trace the neutral motions over 500 times since 1958. Such releases are a simple and reliable method for obtaining horizontal velocities with good accuracy and height resolution. Deriving the diffusion characteristics is more difficult but two detailed studies of the expansion rates have been carried out. Analyses from the earlier experiments show enhanced or anomalous diffusion rates in a 10 to 15 km altitude range above the turbopause. (MAJOR)</font></p> <p> <font size="3">Even if only partially successful, this study is expected to contribute significantly to our understanding of turbulent motions in the atmosphere as turbulence at small scales is currently poorly understood. (MINOR)</font></p> <p> &nbsp;</p>
Thermosphere-Ionosphere Modeling with Forecastable Inputs: Case Study of the June 2012 High Speed Stream Geomagnetic Storm
This is the companion dataset for the Journal paper ”Thermosphere-Ionosphere Modeling With Forecastable Inputs: Case Study of the June 2012 High Speed Stream Geomagnetic Storm” (under review). The dataset contains raw outputs from a global ionosphere-thermosphere model for a geomagnetic storm events. The outputs are in IDL binary format, containing the model solution of the total electron content, the magnetic field, density, velocity, and temperature for neutral and ion species. The outputs are analyzed in the paper to evaluate the forecast capability of the model.
Development of a Robust Low-Power Pressure Transducer for Thermospheric Applications Project
<p> The Earth&rsquo;s ionosphere is home to a number of phenomena that are regularly observed but still unpredictable; obvious examples include equatorial spread F, tidal ion layers, and sporadic E. The fundamental connection between these disparate events is that all three are strongly influenced by coupling between ionized and neutral particles. Most of what we know about these phenomena comes from plasma diagnostics &ndash; we can accurately measure electric fields, plasma density, and plasma temperatures in the ionosphere using <em>in-situ </em>probes, ground-based radars, and optical remote sensing techniques. Our ability to measure the neutral temperatures, densities, and motions at ionospheric altitudes is significantly less mature. We therefore propose to develop a low-power transducer system that will enable accurate measurements of neutral pressure and winds when assimilated into existing instrumentation systems. The low power aspect of this transducer concept is particularly important, since it is compatible with very small satellite platforms such as CubeSats. When deployed on constellations of small satellites in different orbit planes, instruments built around the small sensors we develop will be capable of providing simultaneous global measurements of neutral pressures and winds. These measurements will produce marked improvements in our predictive models, and bring us one step closer to forecasting the diverse phenomena that arise due to ion-neutral interactions in the upper atmosphere.</p>
Sounding rocket payload systems for in-situ measurements of ionosphere-thermosphere structure at small spatial scales Project
<p> The methodology developed under this grant is primarily an effort to develop new sub-payload technologies and an inexpensive method of testing them. The three technical goals are: (1) to improve and test the existing spring sub-payload ejection system and rocket propelled ejection system, (2) to test the performance of ampule-deployed radar chaff (rather than TMA) to track high altitude winds, and (3) to develop and test sensor and telemetry packages to monitor the attitude stability and position of deployed sub-payloads.&nbsp; The proposed effort will also demonstrate very low cost, low altitude rockets as an inexpensive flight test of payloads prior to expensive sounding rocket deployments. The payloads tested on 5 to 7 low-cost rockets will be (1) foil chaff designed for radar tracking of mesospheric winds, (2) plasma instruments composed of GPS monitors, magnetometers, and accelerometers, and (3) android phones for the investigation of off-the-shell instrumentation and telemetry.&nbsp; Finally, a campaign of 2 to 4 sounding rocket deployments on &lsquo;as-available&rsquo; flights from Poker Flats will be used to test spring ejection without spin up, spring ejection with spin up for sub-payload attitude control, and rocket ejection</p>
Infrared Interferometry of Auroral Ionosphere-Thermosphere Energetics Project
<p> <span style="font-size: 12px;"><span style="font-family: times new roman,times,serif;">&nbsp;The FWMI prototype development is underway at USU/SDL. To develop the FWMI, USU/SDL is leveraging the successful implementation of a rocket-borne Michelson interferometer/spectrometer system that was designed by USU/SDL in the early 1980s and flown multiple times on sounding rockets. This sensor was designated the Rocket-Borne Field-Widened Interferometer-II (RBFWI-2). Utilizing modern designs, technologies, and components, the new prototype FWMI will significantly enhance the original RBFWI-2 to meet three technical goals: (1) extended spectral coverage, (2) higher spectral resolution, and (3) extended dynamical range. USU/SDL also intends to achieve large reductions in mass, volume, and power. The resultant prototype FWMI will then be a pathfinder for future missions that focus on addressing key scientific objectives and critical supporting science questions in auroral ionosphere-thermosphere energetics.</span></span></p> <p class="Default" style="margin: 0in 0in 0pt;"> <span style="font-size: 12px;"><span style="font-family: times new roman,times,serif;"><font color="#000000">The successful flight of RBFWI-2 established a solid foundation for the development of the prototype FWMI. Based on that heritage, the current effort focuses on the development of a new optical detector system, a new sensor signal-conditioning system based on modern electronics, as well as extending the displacement of the optics to increase spectral resolution. These new techniques and other modern technologies will be added to the proven RBFWI-2 legacy design to allow the prototype FWMI to serve as the foundation for a flight FWMI version capable of meeting the targeted instrument specifications that are summarized below: </font></span></span><span style="font-size: 11.5pt;"><font color="#000000"><font face="Times New Roman"><o:p></o:p></font></font></span></p> <p class="Default" style="margin: 0in 0in 1.6pt;"> <span style="font-size: 12px;"><span style="font-family: times new roman,times,serif;"><font color="#000000">1. Spectral bandpass of 1300-8100 cm-1 </font></span></span><font color="#000000"><font face="Times New Roman"><span style="font-size: 8pt;"><o:p></o:p></span></font></font></p> <p class="Default" style="margin: 0in 0in 1.6pt;"> <span style="font-size: 12px;"><span style="font-family: times new roman,times,serif;"><font color="#000000">2. Spectral resolution of &le; 1.0 cm-1 </font></span></span><font color="#000000"><font face="Times New Roman"><span style="font-size: 8pt;"><o:p></o:p></span></font></font></p> <p class="Default" style="margin: 0in 0in 0pt;"> <span style="font-size: 12px;"><span style="font-family: times new roman,times,serif;"><font color="#000000">3. Dynamic range characterized by a 10-13 W cm-2 sr-1(cm-1)-1 NER. </font></span></span><font color="#000000"><font face="Times New Roman"><span style="font-size: 11.5pt;"><o:p></o:p></span></font></font></p>
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Viewing Direction A 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.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction B
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
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 Wind Vectors Green
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 A
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 A
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.
ADAPTIVE MODEL REFINEMENT FOR THE IONOSPHERE AND THERMOSPHERE
ADAPTIVE MODEL REFINEMENT FOR THE IONOSPHERE AND THERMOSPHERE ANTHONY M. D’AMATO∗, AARON J. RIDLEY∗∗, AND DENNIS S. BERNSTEIN∗∗∗ Abstract. Mathematical models of physical phenomena are of critical importance in virtually all applications of science and technology. This paper addresses the problem of how to use data to improve the fidelity of a given model. We approach this problem using retrospective cost optimization, a novel technique that uses data to recursively update an unknown subsystem interconnected to a known system. Applications of this research are relevant to a wide range of applications that depend on large-scale models based on firstprinciples physics, such as the Global Ionosphere-Thermosphere Model (GITM). Using GITM as the truth model, we demonstrate that measurements can be used to identify unknown physics. Specifically, we estimate static thermal conductivity parameters, and we identify a dynamic cooling process.
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