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42 results for “upper atmosphere”
Mountain waves in the upper atmosphere of Venus
<p>This dataset contains the GCM reduced variables of the outputs of the Venus PCM for the manuscript "Mountain waves in the upper atmosphere of Venus". It consists of NetCDF files showed in the following figures:</p> <p>Figure 1. Zonal wind and wave amplitude above the Beta Regio area [100◦W-40◦W ; 30◦S-30◦N] for three local times.</p> <p>Figure 2. Maps of downwards vertical wind speed (cm/s) above Beta Regio from the cloud top (70 km) to the thermosphere (135 km) for three local times. Positive (negative) values are downwards (upwards).</p> <p>Figure 3. Westward zonal wind (averaged for latitudes 40◦S-40◦N for data accumulated over one solar day) as a function of local time for altitudes 100 and 135 km. Continuous lines are averaged for one solar day, whereas the dashed line is averaged only for local times 16h-18h above Beta Regio (longitude 78◦ W). </p> <p>Figure 4. Vertical wind speed for local times 14h-16h and all latitudes, in m/s above the cloud top.</p>
Phosphorus Chemistry in the Earth's Upper Atmosphere
<p><strong>Phosphorus Chemistry in the Earth’s Upper Atmosphere</strong></p> <p>by</p> <p>John M.C. Plane<sup>1*</sup>, Wuhu Feng<sup>1,2</sup> and Kevin M. Douglas<sup>1</sup></p> <p><sup>1</sup> School of Chemistry, University of Leeds, UK</p> <p><sup>2</sup> National Centre for Atmospheric Science and School of Earth and Environment, University of Leeds, UK</p> <p> </p> <p>The repository contains the data used in the above paper.</p>
Data and scripts for GRL article: Author's reply to Comment by Greaves et al. on ``Phosphine in the Venusian Atmosphere: A Strict Upper Limit from SOFIA GREAT Observations''
<p>Python scripts and raw SOFIA Data to reproduce the figures found in GRL article: Author's reply to Comment by Greaves et al. on ``Phosphine in the Venusian Atmosphere: A Strict Upper Limit from SOFIA GREAT Observations''</p>
Dataset of "Effects of latitude-dependent gravity wave source variations on the middle and upper atmosphere"
<p>This is a dataset for three 60-day simulations with the CMAT2-GCM for June-July 2010 conditions, using the Whole atmosphere gravity wave parameterization by Yiğit et al. (2008).</p> <p>Dimensions: 66 vertical levels, 24 longitudes, and 91 latitudes. The bottom level is at 100 mb. </p> <p>Variables: There are seven physical variables. Daily-averaged zonal wind, temperature, geopotential height, zonal drag, gravity wave total heating/cooling rate, gravity wave-induced temperature fluctuations, and gravity wave absolute momentum flux. </p> <p>Simulations: A benchmark run "00n", a run with latitude-dependent gravity wave source spectrum with 50% increased flux at the lower boundary in both hemispheres "51n"; same as "52n" but 100% increased flux in the Southern Hemisphere only. </p>
The oxygen isotope compositions of large numbers of small cosmic spherules: Implications for their sources and the isotopic composition of the upper atmosphere
<p>Cosmic spherules are micrometeorites that melt at high altitude as they enter Earth's atmosphere and their oxygen isotope compositions are partially or completely inherited from the upper atmosphere, depending on the heating experienced and the nature of their precursor materials. In this study, the <b>three oxygen isotope</b> compositions of 137 <b>cosmic spherules are</b> determined using 277 in-situ analyses by ion probe. Particles of each different type of cosmic spherule (scoriaceous, porphyritic, cryptocrystalline, barred, glass, calcium aluminium and titanium (CAT), G-type and I-type) in the diameter range ~52–480mm were analysed. The results confirm that the <b>three</b> oxygen isotope compositions of melted <b>micrometeorites</b> reflect a combination of their precursor composition, exchange with the atmosphere and mass fractionation owing to evaporation during entry heating. The data <b>appear to </b>reveal an increase in average δ<sup>18</sup>O values of silicate dominated (S-type) spherules in the series scoriaceous<porphyritic<barred<glass<CAT spherules (~20, 22, 25, 26 and 50‰) that is consistent with the evolution of oxygen isotopes by mass fractionation owing to increased average entry heating. The trend of δ<sup>17,18</sup>O is broadly parallel to the terrestrial fractionation line and thus suggests mass fractionation dominates changes in isotopic composition, with atmospheric exchange a less significant effect. The D<sup>17</sup>O values of spherules, therefore, are mostly preserved and suggest that ~80% of particles are related to the carbonaceous chondrites (CC) and are probably samples of C-type asteroids. The genetic relationships between different S-types can also be determined with scoriaceous, barred and cryptocrystalline spherules mostly having low D<sup>17</sup>O values <b>(≤0‰)</b> suggesting they are mainly derived from CC-like sources, whilst porphyritic mostly have positive D<sup>17</sup>O <b>(>0‰)</b> suggesting they are largely from ordinary chondrite (OC)-like sources related to S(IV)-type asteroids. Glassy and CAT-spherules have D<sup>17</sup>O values <b>indicating</b> they formed by intense entry heating of both CC and OC-like materials. I-type cosmic spherules have a narrow range of δ<sup>17</sup>O (~20–25‰) and δ<sup>18</sup>O (~38–48‰) values, with D<sup>17</sup>O (~0‰) <b>suggesting</b> their oxygen is obtained entirely from the Earth's atmosphere, albeit with significant mass fractionation owing to evaporation during entry heating. The observed range of δ<sup>18</sup>O with the size is suggested here to reflect entry angle with high values representing enhanced heating at high angle. Finally, G-type <b>cosmic spherules</b> have unexpected isotopic compositions suggesting little mass-fractionation from a CC-like source and are suggested to have sulphide-silicate precursors with relatively low melting temperatures. The results of this study provide a <b>vital assessment</b> of the <b>wider</b> population of extraterrestrial dust arriving <b>at the</b> Earth.</p>
Data from: Upper atmosphere heating from ocean-generated acoustic wave energy
Colliding sea surface waves generate the ocean microbarom, an acoustic signal that may transmit significant energy to the upper atmosphere. Previous estimates of acoustic energy flux from the ocean microbarom and mountain/wind interactions are on the order of 0.01 to 1 mW/m2, heating the thermosphere by tens of degrees Kelvin per day. We captured up going ocean microbarom waves with a balloon borne infrasound microphone; the maximum acoustic energy flux was approximately 0.05 mW/m2. This is about half the average value reported in previous ground-based microbarom observations spanning eight years. The acoustic flux from the microbarom episode described here may have heated the thermosphere by several degrees Kelvin per day while the source persisted. We suggest that ocean wave models could be used to parameterize acoustically-generated heating of the upper atmosphere based on sea state.
Local to regional methane emissions from the Upper Silesia Coal Basin (USCB) quantified using UAV-based atmospheric measurements
<p>Raw data for Andersen et al., 2021 (Local to regional methane emissions from the Upper Silesia Coal Basin (USCB) quantified using UAV-based atmospheric measurements)</p>
Northern hemispheric atmospheric ethane trends in the upper troposphere and lower stratosphere (2006-2016) with reference to methane and propane
<p>Datasets for northern hemispheric atmospheric ethane, propane and methane (2006-2016) from airborne measurements by IAGOS-CARIBIC project. </p>
Thermal Structure of the Martian Upper Atmosphere from MAVEN NGIMS
<p>This repository contains data to accompany the publication of our manuscript, "Thermal Structure of the Martian Upper Atmosphere from MAVEN NGIMS" which appears in the Journal of Geophysical Research: Planets.</p> <p>The repository contains .mat files of NGIMS densities and temperatures, as well as associated ephemerides. The filenames have the following structure,</p> <p> </p> <p>mvn_ngi_s3_BIN#_YYYYMMDDtoYYYYMMDD_TID##toTID##_ORBITtoORBIT.mat.</p> <p> </p> <p>Each .mat file contains a MATLAB struct named s3. Each s3 struct contains arrays of TIDs, orbits, dates, filenames of data products used to construct the s3, and periapsis information for each orbit. Mean profiles of detector counts and count rates, Ar, CO2, and N2 densities, density corrections, temperatures derived from the densities, altitude, latitude, longitude, local time, solar zenith angle, Ls, heliocentric distance, spacecraft position and velocity, solar latitude and longitude, and NGIMS ram angle are also included. In the "pass" struct within each s3 struct, there are data for each individual orbit in the s3 file. That is, the pass structure contains the data from each orbit which has been binned to obtain the mean profiles in the s3 struct. The pass struct is accessed by commands of the form,</p> <p> </p> <pre><code>s3.pass(n).FIELD</code></pre> <p> </p> <p>where n is an integer between 1 and length(s3.orbit) indicating the orbit in s3.orbit or TID in s3.tid to be accessed and FIELD the field, such as den_Ar (Ar density) or tmp_Ar (Ar temperature), to be accessed.</p> <p> </p> <p>For more information, please contact the corresponding author of the manuscript.</p>
Data Products for "The Upper Atmosphere of Uranus from Stellar Occultations II: Revised Temperatures in the Upper Stratosphere and Lower Thermosphere"
<p>From the README file:</p> <p>Organization of data products connected to Saunders et al. (2023, PSJ) and Saunders et al. (2024, PSJ).</p> <p>/forward_modeling_results.csv -- Anderson-Darling test values and critical values for each comparison between Voyager 2 profiles and observed stellar occultation light curves. Voyager 2 profiles were forward modeled into stellar occultation light curves to enable a direct comparison to observed, Earth-based stellar occultation profiles using the Anderson-Darling test of normality. Critical values are provided. See Section 3 of Saunders+23 and Section 2 of Saunders+24.</p> <p>/original_occultation_profiles/ -- Previously published atmospheric profiles from Earth-based stellar occultations. Data were extracted using a data extraction software on published papers. The citation for each data source is provided below. <br>/original_occultation_profiles/1977* -- Elliot et al. (1979)<br>/original_occultation_profiles/1981* -- French et al. (1983)<br>/original_occultation_profiles/1982-04* -- Sicardy et al. (1985)<br>/original_occultation_profiles/1982-05* -- French et al. (1987)<br>/original_occultation_profiles/1983* -- Elliot et al. (1987)</p> <p>/reprocessed_occultation_profiles/ -- All atmospheric profiles resulting from reprocessing the 26 occultation profiles.<br>/reprocessed_occultation_profiles/profiles/ -- Only the atmospheric profiles.<br>/reprocessed_occultation_profiles/profiles/* -- Each individual profile, in original vertical resolution. Columns: radius [km] (from center of Uranus), temperature [k], pressure [microbar], number density [m^-3], refractivity, scale_height [km] (pressure scale height H = kT/mg), y [km] (close-approach distance of the line connecting the viewer and the occulted star to the center of Uranus, see Saunders+23 for description). Units are provided in column headers.<br>/reprocessed_occultation_profiles/errors/ -- Only the errors for the atmospheric profiles.<br>/reprocessed_occultation_profiles/errors/* -- 1-sigma srrors for each individual profile.</p> <p>/atmospheric_models/ -- One-dimensional atmospheric model products. See Section 5 of Saunders+24.<br>/atmospheric_models/model_parameters/model_constants -- Values of constants used in the models. See Table 3 of Saunders+24.<br>/atmospheric_models/model_parameters/model_parameters -- Values and uncertainties of model parameters. See Table 3 of Saunders+24.<br>/atmospheric_models/model_profiles/* -- Profiles for the 9 models provided in Appendix C of Saunders+24. "Average" profiles are fit to the average of the 26 reprocessed stellar occultations; "cool" profiles are fit to the lower bound of the reprocessed occultations; "warm" profiles are fit to the upper bound of the reprocessed occultations. "Best-fit" profiles are the best fit model results; "lower" profiles are the lower bound of the family of generated profiles, meant to serve as a range of uncertainty; "upper" profiles are the upper bound. See Table 3 and Appendix C in Saunders+24 for more information. Units are provided in column headers.</p> <p> </p>
Data from: Upper atmosphere heating from ocean-generated acoustic wave energy
Open the record for dataset details and reuse information.
The oxygen isotope compositions of large numbers of small cosmic spherules: Implications for their sources and the isotopic composition of the upper atmosphere
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The effects of the upper atmosphere and corona on the solar wind interaction with Venus
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Data for "Martian oxygen and hydrogen upper atmospheres responding to solar and dust storm drivers: Hisaki space telescope observations"
<p>Data files (.npy) and python codes (.ipynb) to produce the figures in the paper.</p> <p>Download the zip file (dataforfigures_v2.zip), open plot_figX.ipynb with Jupyter notebook, and run it.</p> <p> </p>
Supplement videos for manuscript Impacts of storm "Zyprian" on middle and upper atmosphere observed from Central European stations
<p>Supplement video material for the manuscript Impacts of storm “Zyprian” on middle and upper atmosphere observed from Central European stations. It contains loop of MSG satellite observation and infrasound animations.</p>
Climate Changes in the Upper Atmosphere: Contributions by the Changing Greenhouse Gas Concentrations and Earth's Magnetic Field
<p>These are data that were used to write the paper: "Climate Changes in the Upper Atmosphere: Contributions by the Changing Greenhouse Gas Concentrations and Earth's Magnetic Field " by Liying Qian, Joseph M. McInerney, Stan S. Solomon, Hanli Liu, Alan G. Burns.</p>
Martian Dust Storms and Gravity Waves: Disentangling Water Transport to the Upper Atmosphere
<p>The data for JGR:Planets article figures.</p>
Chemical species in Titan's upper atmosphere observed by Cassini/UVIS stellar occultations
<p>The archive files contain the line-of-sight abundances and local densities of CH<sub>4</sub>, C<sub>2</sub>H<sub>2</sub>, C<sub>2</sub>H<sub>4</sub>, C<sub>2</sub>H<sub>6</sub>, C<sub>4</sub>H<sub>2</sub>, C<sub>6</sub>H<sub>6</sub>, HCN, HC<sub>3</sub>N, and haze particles in Titan's upper atmosphere retrieved using Cassini/UVIS stellar occultation observations during 18 Titan flybys. These results are shown in Figures 5-10 of the manuscript listed below.</p> <p>Fan, S., Zhao, D., Li, C., Shemansky, D. E., Liang, M. -C., and Yung, Y. L. (2022) Seasonal Variations of Chemical Species in Titan’s Upper Atmosphere. <em>The Planetary Science Journal.</em></p>
NACP MCI: Tower Atmospheric CO2 Concentrations, Upper Midwest Region, USA, 2007-2009
This data set provides high precision and high accuracy atmospheric CO2 data from seven instrumented communication towers located in the U.S. Upper Midwest. The overall sampling period was from January 2007 through December 2009 although actual sampling dates vary within this time period for individual towers and sampling heights above ground level. The measurements were obtained in support of the North American Carbon Program (NACP) Mid-Continent Intensive (MCI) campaign.The sampling network included: the five Ring 2 towers (Centerville (Iowa), Galesville (Wisconsin), Kewanee (Illinois), Mead (Nebraska), and Round Lake (Minnesota)) deployed and operated by PSU; the Missouri Ozarks (Missouri) co-located AmeriFlux site (PSU/Oak Ridge National Laboratory (ORNL)); and the Rosemount (Minnesota) tall tower trace gas observatory (University of Minnesota, Rosemount Research and Outreach Center (RROC)). Hourly CO2 dry mole fractions (in ppm) were averaged from measurements made at different above-ground levels on the towers and are reported in Coordinated Universal Time (UTC). For the five Ring 2 sites, daily daytime average CO2 dry mole fractions were also calculated, from hourly values between 12:00-17:00 local standard time and reported in UTC. There are seven compressed (.zip) data files and one comma-separated (.csv) file with this data set. Data quality flags are provided in each file.
Ground-Based GNSS-based Upper Atmospheric Realtime Disaster Information and Alert Network (GUARDIAN) Galileo daily accumulated real-time Precise Orbit Determination (POD) Clock Corrections (60-second sampling, 24-hour files) from NASA CDDIS
This product contains a time series of clock biases for healthy satellites in the Galileo constellation that are accumulated every minute throughout the day. In addition, formal 1-sigma uncertainties for the corrections are provided. The product is generated at JPL's Global Differential GPS Operations Centers in real-time. The data in this product can be concatenated with other daily products to provide larger coverage in time.
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Allen Brain Atlas
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Annotated Behaviour and Observability Dataset (ABODe)
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.