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6 results for “Titan's atmosphere”
GCMS Huygens Dataset and methane mole fraction in Titan atmosphere
<p>This archive contains the dataset relative to the publication "Reanalaysis of the Huygens GCMS dataset: I. High resolution<br>Methane vertical profile in Titan atmosphere" by Gautier et al. in A&A 2024.<br>The entire set of recalibrated GCMS data is provided and includes the GCMS level 3 data product generated during this work.<br>Following the nomenclature of the GCMS data archived on the PDS this file is named GCMS_1US_STG3.TAB. The associated file<br>GCMS_1US_STG3.FMT contains a description of each column following the existing archived format. An additional information<br>in the description using the keyword "CHANGED_STG2_3" indicates whether or not the column was modified between STG2 and<br>STG3 compared to the dataset retrieved on the PDS.<br>The molefractions.csv table contains the retrieved methane mixing ratio through the atmospheric column. First column is the<br>time since beginning of GCMS measurements. Column 2, 3 and 4 are the altitude, atmospheric pressure and temperature, respec-<br>tively, from HASI measurements for the corresponding time stamp. Column 5 and 6 are the retrieved methane mole fraction and its<br>standard deviation. For altitudes comprised between 146 and 30 km, data has been binned to a kilometric resolution to enhance S/N.<br>The associated values for time, altitude, pressure and temperature correspond to the average value of the bin in the GCMS and HASI<br>data. Associated methane mole fraction corresponds to the retrieved value for the binned data. From 30 km and below, we used the<br>native GCMS vertical resolution. In this range, timestamps correspond to the exact time of each measurement according to GCMS<br>clock. Corresponding altitude, pressure and temperature were calculated using a linear interpolation between the two nearest HASI<br>points. Reported methane mole fractions and uncertainties correspond to the retrieved values for each altitude smoothed using a 10<br>points moving median.</p>
Gravity waves in Titan's atmosphere: A comparison between linearized wave model calculations and HASI observations
<p>The data for the article "Gravity waves in Titan's atmosphere: A comparison between linearized wave model calculations and HASI observations" (GWTA). </p> <p> </p> <ol> <li>"Titan_CJP_std_chem.dat" is the background atmosphere data of Titan's atmosphere from Strobel's model. It is used in Figure 1 of the article.</li> <li>"HASI_T_p_rho_vsZ_2008.dat" is the data for Cassini-Huygens observations in Titan's atmosphere. It is used in Figure 1 of the article.</li> <li>"Mma-Program-for-GW-on-Titan.txt" is the main Mathematica program to simulate the gravity waves on Titan.</li> <li>"solutions-fun.rar" is the simulation result. This RAR file includes 174 gravity wave samples simulated with different periods and horizontal wavelengths (can be read from the subfile names after uncompressing). These gravity wave solutions are stored as InterpolatingFunction of Mathematica. The solution describes the gravity wave temperature, velocity, and density perturbations profiles from altitude 300km to 2000km. However, they are plain texts and can easily be read by any software. Figures from 2-10 are based on these data.</li> </ol> <p> </p>
Dataset for "Air-sea interactions on Titan: effect of radiative transfer on the lake evaporation and atmospheric circulation"
<p>These documents are supplements to the "Air-sea interactions on Titan: effect of radiative transfer on the lake evaporation and atmospheric circulation" paper published by the same authors in The Planetary Science Journal in 2022.</p> <p>Are made available:</p> <p>-the Supporting Information document on the performed sensitivity study,<br> "paper_mtWRF_lake_RT_220825_SI.pdf"</p> <p>-the Fortran source code of the radiative transfer module developed for this work,<br> "module_ra_gray.F"</p> <p>-all the netCDF simulation outputs and a list describing their parameters,<br> "run-##.nc.gz"<br> "list_simulations_2D_paper2022_RT_zenodo.pdf"</p> <p>-the Python codes to plot figures from the netCDF output files,<br> "mtwrf_analysis_#D_#.py"</p>
RT Dataset -- Updated radiative transfer model for Titan in the near-infrared wavelength range: Validation against Huygens atmospheric and surface measurements and application to the Cassini/VIMS observations of the Dragonfly landing area
<p>This dataset contains all Radiative Transfer (RT) results made for the paper.</p> <p>The data are stored in 5 zipped-folders names with the Cassini/VIMS cube flyby and id, or explicitly for Huygens/ULIS calibrated observations:</p> <ul> <li>TB_C1481624349_1</li> <li>T40_C1578266417_1</li> <li>T38_C1575509158_1</li> <li>T40_C1578263500_1</li> <li>T40_C1578263152_1</li> <li>ULIS_observations</li> </ul> <p>The TB_C1481624349_1 folder contains the Cassini/VIMS cube over HLS, the HLS end-member (End_member.txt), the surface albedo retrieved by Karkoschka et al. (2016) corrected for the photometry (HLS_Karkoschka_2016_spectrum.txt), and the inverted surface albedo (Surface_albedo.txt).</p> <p>In these folders, each VIMS pixel is stored in a .txt file with the following pattern:</p> <p><CUBE_ID>_<PIXEL_SAMPLE>_<PIXEL_LINE> .txt</p> <p>It starts with a header describing the observation: </p> <ul> <li>CUBE_ID: the VIMS cube id (`C1234567890_1` format)</li> <li>SAMPLE: the pixel sample number.</li> <li>LINE: the pixel line number.</li> <li>LONG: the pixel longitude (in degree).</li> <li>LAT: the pixel latitude (in degree).</li> <li>INC: the surface incident angle (in degree).</li> <li>EMI: the surface emergent angle (in degree).</li> <li>PHASE: the surface phase angle (in degree).</li> </ul> <p>For the Selk crater cubes (T40_C1578266417_1, T38_C1575509158_1, T40_C1578263500_1, T40_C1578263152_1), the header also contains the spatial sampling and the radiative transfer model outputs: </p> <ul> <li>Spatial sampling (km/pix).</li> <li>Fh: the haze scaling factor.</li> <li>Fm: the mist scaling factor.</li> <li>1-sigma (Fh): the 1-sigma uncertainty on Fh.</li> <li>1-sigma (Fm): the 1-sigma uncertainty on Fm.</li> <li>Reduced chi2: the reduced chi2. </li> </ul> <p>Then contains the observed spectra:</p> <ul> <li>Column 1: the VIMS channel central wavelength (in micrometers).</li> <li>Column 2: the VIMS pixel I/F.</li> <li>Column 3: the VIMS pixel I/F 1-sigma uncertainty. </li> </ul> <p>For the Selk crater cubes (T40_C1578266417_1, T38_C1575509158_1, T40_C1578263500_1, T40_C1578263152_1), 3 columns are added for: </p> <ul> <li>Column 4: the surface albedo.</li> <li>Column 5: the upper 1-sigma uncertainty on the surface albedo.</li> <li>Column 6 : the lower 1-sigma uncertainty on the surface albedo.</li> </ul> <p>The ULIS folder contains the Huygens/ULIS calibrated observations (in I/F) and the simulations with 1-sigma uncertainties as a function of the altitude (in km):</p> <ul> <li>Column 1: the VIMS channel central wavelength (in micrometers), stopped at the end of the Huygens/ULIS wavelength range.</li> <li>Column 2: the ULIS I/F.</li> <li>Column 3 : the simulated I/F.</li> <li>Column 4: the lower 1-sigma uncertainty on the simulation.</li> <li>Column 5 : the upper 1-sigma uncertainty on the simulation.</li> </ul>
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>
Cassini Orbiter RSS Neutral Atmosphere T-P profiles for Titan Bundle
Atmospheric profiles of Titan
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