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121 results for “Titan”
Spherical harmonic models of the shape of Titan
<p>This archive contains spherical harmonic models of the shape of Saturn's moon Titan constructed from data collected by the Cassini mission. Two such models are here archived:</p> <ul> <li>Titan_shape_Mitri2014_unnorm.sh (Mitri et al. 2014)</li> <li>Titan_shape_Corlies2017_unnorm.sh (Corlies et al. 2017)</li> </ul> <p>Both models make use of unnormalized spherical harmonic functions that include the Condon-Shortley phase factor of (-1)^m. The model from Mitri et al. (2014) is developed to spherical harmonic degree 6, whereas the model of Corlies et al. (2017) is developed to degree 8. Note that most gravity models of Titan use spherical harmonic functions that exclude the Condon-Shortley phase factor.</p>
Data set for paper "Ramparts around lakes on Titan impact winds and methane evaporation"
<p>Data and post-processing code used for the paper "Ramparts around lakes on Titan impact winds and methane evaporation", submitted to PSJ in 2024.</p> <p>Are made available:<br> - a list of the simulations (list_simulations_ramparts2D.pdf)<br> - the simulations' netCDF outputs (run-t##.nc.gz)<br> - the input files used to run the simulations (in input_files/)<br> - the post-processing python codes used to plot the figures (in post_processing_codes/)<br> - tables of latent heat flux and horizontal wind values (Tables_LH_and_Uwind.pdf)<br> - a gif of the horizontal wind in the reference run (u_wind_run-t04_speed.gif)<br> - a gif of the vertical wind in the reference run (w_wind_run-t04_speed.gif)</p>
Origin of relaxor behavior in barium titanate based lead-free relaxors
<p>It is well known that disordered relaxor ferroelectrics exhibit local polar correlations. The origin of localized fields that disrupt long range polar order for different substitution types, however, is unclear. Currently, it is known that substituents of the same valence as Ti4+ at the B-site of barium titanate lattice produce random disruption of Ti-O-Ti chains that induces relaxor behavior. On the other hand, investigating lattice disruption and relaxor behavior resulting from substituents of different valence at the B-site is more complex due to the simultaneous occurrence of charge imbalances and displacements of the substituent cation. The existence of an effective charge mediated mechanism for relaxor behavior appearing at low (<10%) substituent contents in heterovalent modified barium titanate ceramics is evinced from this data, which underpin the publication by the same name currently in press by Advanced Electronic Materials. These results will add credits to the current understanding of relaxor behavior in chemically modified ferroelectric materials and also acknowledge the critical role of defects (such as cation vacancies) in lattice disruption, paving the way for chemistry-based materials design in the field of dielectric and energy storage applications</p>
The Titan Seasonally Varying Radiative Species (SVRS) Dataset
<p><strong>Update 17 June 2023: The 'latitude' array is erroneously reversed relative to the 'abundance' array in svrs_molecule.nc. The user should reverse the order of 'latitude' upon reading it. Example: netCDF4.Dataset('svrs_molecule.nc)['latitude'][::-1]. This did not affect Lombardo & Lora (2023).</strong></p> <p>Here is archived the Titan <strong>S</strong>easonally <strong>V</strong>arying <strong>R</strong>adiative <strong>S</strong>pecies (SVRS) dataset, which consists of netCDF files containing trace gas abundances (svrs_molecule.nc) and the aerosol opacity (svrs_haze.nc). SVRS was developed with the intent of providing a single source of seasonal scale climatological information on Titan's radiatively active species from the troposphere through the stratopause. This was accomplished by interpolating between measurements from individual Cassini flybys of Titan where trace gas abundance and aerosol opacity were determined. The trace gases included are C<sub>2</sub>H<sub>6</sub>, C<sub>2</sub>H<sub>4</sub>, C<sub>2</sub>H<sub>2</sub>, p-C<sub>3</sub>H<sub>4</sub>, C<sub>4</sub>H<sub>2</sub>, HCN, and HC<sub>3</sub>N. The trace gas abundances are on 2° latitude, 5° <em>L<sub>s</sub></em> grid, with 99 levels extending from just above the surface to 0.001 Pa. Haze opacity is included for the infrared, visible, and ultraviolet spectral windows, spanning 1 cm<sup>-1</sup> -- 40000 cm<sup>-1</sup>. The haze opacity is on a 2° latitude, 5° <em>L<sub>s</sub></em> grid with 900 levels extending from 10<sup>6</sup> Pa (extrapolated to pressures greater than Titan's surface pressure) to 10<sup>-3</sup> Pa. The methods used to produce SVRS are detailed in Lombardo & Lora (2023), <em>Icarus</em>, doi: j.icarus.2022.115291. </p> <p>This archive also includes simulation data from the Titan Atmospheric Model (TAM), discussed in the above reference. This simulation utilized molecular abundance and aerosol opacity profiles from SVRS to calculate seasonally accurate radiative heating rates. This archive contains zonal means of the simulated zonal and meridional winds, temperature, and the calculated meridional mass stream function. The data are averaged over 10° <em>L<sub>s</sub></em> windows, and sampled every 10° <em>L<sub>s</sub></em> (with 1° <em>L<sub>s</sub></em> corresponding to approximately 1 Earth month), and extends from the surface (1.465×10<sup>5 </sup>Pa) through the lower mesosphere (about 0.01 Pa). An animation of the data included in this netCDF file is included as Lombardo_TAM_2023_data.mp4.</p> <p><strong>We ask that you cite us in your use of the data: Lombardo & Lora (2023), <em>Icarus</em>, doi: j.icarus.2022.115291</strong></p>
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>
Material Property Database of Organic Liquids, Ices, and Hazes on Titan
<p>Titan has a diverse range of materials in its atmosphere and on its surface: the simple organics that reside in various phases (gas, liquid, ice) and the solid complex refractory organics that form Titan's haze layers. These materials all actively participate in various physical processes on Titan, and many material properties are found to be important in shaping these processes. Future in-situ exploration on Titan would likely encounter a range of materials, and a comprehensive database to archive the material properties of all possible material candidates will be needed.</p> <p>Here we archive several important material properties of the organic liquids, ices, and the refractory hazes on Titan that are available in the literature and/or that we have computed. These properties include thermodynamic properties (phase change points, sublimation and vaporization saturation vapor pressure, and latent heat), physical property (density), and surface properties (liquid surface tensions and solid surface energies).</p> <p>We have archived all the data involved in our first paper (https://arxiv.org/abs/2210.01394 for the Arxiv version and https://doi.org/10.3847/1538-4365/acc6cf for the publisher version) here to make them available to the science community. These data can be used as inputs for various theoretical models to interpret current and future remote sensing and in-situ atmospheric and surface measurements on Titan. The material properties of the simple organics may also be applicable to giant planets and icy bodies in the outer solar system, interstellar medium, and protoplanetary disks.</p> <p>The "Summary of Data Tables and Jupyter Notebook Files" summarizes the names of all the data files (.csv) and Jupyter Notebook files (.ipynb) and their corresponding Tables in the paper.</p> <p><strong>Please cite our paper in your use of the data: Yu et al. (2023), https://doi.org/10.3847/1538-4365/acc6cf</strong></p> <p><strong>Yu, X., Yu, Y., Garver, J., Li, J., Hawthorn, A., Sciamma-O’Brien, E., ... & Barth, E. (2023). Material Properties of Organic Liquids, Ices, and Hazes on Titan. The Astrophysical Journal Supplement Series, 266(2), 30.</strong></p>
The propagation of gravity waves in Titan's stratosphere
<p>The model code and figure data of our article "The propagation of gravity waves in Titan's stratosphere". <a href="https://zenodo.org/api/files/a647c3b7-0796-4a3a-96bc-779957496aad/GW-simulation-program.txt">GW-simulation-program.txt</a> is the Mathematica code used to simulate gravity wave propagation. <a href="https://zenodo.org/api/files/a647c3b7-0796-4a3a-96bc-779957496aad/simulations-nowind.rar">simulations-nowind.rar</a> and <a href="https://zenodo.org/api/files/a647c3b7-0796-4a3a-96bc-779957496aad/simulations-wind.rar">simulations-wind.rar</a> are the simulation results for gravity wave with its horizontal propagation direction perpendicular or not perpendicular to the background wind, respectively. <a href="https://zenodo.org/api/files/a647c3b7-0796-4a3a-96bc-779957496aad/FigureData.rar">FigureData.rar</a> contains several data files for figures in our article.</p>
Cryogenic hyperabrupt strontium titanate varactors for sensitive reflectometry of quantum dots
<p>Supplementary Data for:</p> <p>"Cryogenic hyperabrupt strontium titanate varactors for sensitive reflectometry of quantum dots"</p> <p>Rafael S. Eggli, Simon Svab,Taras Patlatiuk, Dominique Trüssel, Miguel J. Carballido, Pierre Chevalier Kwon, Simon Geyer, Ang Li,<br> Erik P. A. M. Bakkers, Andreas V. Kuhlmann, and Dominik M. Zumbühl</p>
Vertical Compositional Variations of liquid hydrocarbons in Titan's Alkanofers
<p>This data set is composed of six archives (.TAR) which collect input and output files from GROMACS (2018 version) simulations on binary and ternary mixtures representative of liquids in Titan's alkanofers:<br> 3000CH4+1000C2H6+1000N2_90K.tar<br> 3000CH4+1000C2H6+1000N2_95K.tar<br> 4000CH4+1000C2H6_90K.tar<br> 4000CH4+1000C2H6_95K.tar<br> 4000CH4+1000N2_90K.tar<br> 4000CH4+1000N2_95K.tar</p> <p>The system under study is always composed of 5000 molecules. Simulations at 90 K correspond to a pressure of 1.5 bar while those at 95K correspond to a pressure of 120 bar.</p> <p>Each archive contains 5 directories:</p> <p>1)<strong> INPUTS:</strong> It contains all the GROMACS input files (.GRO, .ITP, .TOP) needed to build the simulation box as well as the files required to prepare the molecular dynamics (MD) simulations (.MDP and .TPR). More details about the content of these files is available in the GROMACS manual (https://www.gromacs.org/).<br> 2 README files are added to inform the reader on useful GROMACS commands used here:<br> - README_box.txt: commands to build the simulation box.<br> - README_NVT+NPT-runs.dat: commands to run MD simulations and treat some data.</p> <p>2) <strong>NVTOUT_EQ</strong>: It contains all the files related to the 1-ns NVT equilibration phase, namely, the script for job submission (.SH) together with the related standard ouput files (.OUT and .ERR), and typical GROMACS output files (.GRO, .LOG, .EDR, .TRR, .CPT).<br> Post-treatment data are collected in 2 files:<br> - stats_nvt-eq.dat: Average potential energy, kinetic energy, total energy, temperature and pressure.<br> - energy_nvt-eq.xvg: Potential energy (col. 2), kinetic energy (col. 3), total energy (col. 4), temperature (col. 5), and pressure (col. 6) as a function of time (col.1).</p> <p>3) <strong>NPTOUT_EQ</strong>: It contains the same kind of files as NVTOUT_EQ but for the first 9 ns of the 19-ns NPT equilibration phase.<br> Post-treatment data are collected in 2 files:<br> - stats_npt-eq.dat: Average potential energy, kinetic energy, total energy, temperature, pressure, volume, density, and enthalpy.<br> - energy_npt-eq.xvg: Potential energy (col. 2), kinetic energy (col. 3), total energy (col. 4), temperature (col. 5), and pressure (col. 6), volume (col.7), density (col.8), and enthalpy (col. 9) as a function of time (col. 1).</p> <p>4) <strong>NPTOUT_EQ-RERUN1</strong>: It contains the same kind of files as NPTOUT_EQ but for the last 10 ns of the 19-ns NPT equilibration phase.</p> <p>5) <strong>NPTOUT_ACC</strong>: It contains the same kind of files as NPTOUT_EQ but for the 10-ns NPT accumulation phase. Additional data files also provide diffusion coefficients and shear viscosities depending on the mixture under consideration (see below).</p> <p><em>For binary mixtures</em>, the mean squared displacements (MSD) of species and the corresponding diffusion coefficients are estimated with the "gmx msd" GROMACS command.<br> Data are collected in two files:<br> - msd-CH4.xvg / msd-C2H6.xvg / msd-N2.xvg: MSD (col. 2) as a function of time (col. 1). The value of the corresponding diffusion coefficient (in cm<sup>2 </sup>s<sup>-1</sup>) is indicated as a comment in the preamble of these files.<br> - DCH4.dat / DC2H6.dat / DN2.dat: Estimated diffusion coefficient (in cm<sup>2 </sup>s<sup>-1</sup>) for the three moelcules under study.</p> <p><em>For ternary mixtures</em>, transverse current autocorrelation functions (TCAF) are computed with the "gmx tcaf" GROMACS command to get values of the shear viscosity:<br> - tcaf-slurm.sh, tcaf.out tcaf.xvg. tcaf_all.xvg, tcaf_cub.xvg, tcaf_fit.xvg: script (.SH) and several output files with transverse current autocorrelation functions (.XVG).<br> - visc_k.xvg: shear viscosity (col.2) as a function of the wave number (col.1). The last four viscosities can be fitted to get the shear viscosity at infinite wavelength (see GROMACS manual).</p>
Spherical harmonic models of the gravity field of Titan
<p>This archive contains previously published models of the gravitational field of Saturn's moon Titan.</p> <ul> <li>Durante2019.sh</li> </ul> <p>All models make use of unnormalized spherical harmonic functions that exclude the Condon-Shortley phase factor of (-1)^m.</p>
MicroED datasets of biotin collected on Titan Krios G4 operated at 300kV and Ceta-D camera
<p>MicroED datasets of biotin microcrystals were collected using Titan Krios G4 (300 kV) with the CMOS camera Ceta-D. The stage was controlled using SerialEM and diffraction images were independently collected using Velox software. For this reason, only frames with constant rotation speed should be used for data processing.</p> <p>Rotation step (continuous) was ~0.96°/frame and each dataset consisted of ~63 images (tilt range is +/-30°). The calibrated camera lengths using <a href="https://www.tedpella.com/calibration_html/TEM_STEM_Test_Specimens.htm">evaporated aluminum</a> were 751.09 mm, 952.85 mm, and 1075.09 mm, corresponding to nominal lengths of 430 mm, 540 mm, and 610 mm, respectively. Biotin crystals belonged to space group <em>P</em>2<sub>1</sub>2<sub>1</sub>2<sub>1</sub> with a~5.2, b~10.2, c~20.8 Å, and could be merged at ~0.6 Å resolution.</p> <p>Collection conditions:</p> <ul> <li>gun lens 5, spot 11, C2 aperture 20, beam size 1.5 μm, 0.033 e/Å<sup>2</sup>/sec</li> </ul> <p>Note:</p> <ul> <li>emd files (hdf5 format) were transparently compressed using h5repack -f SHUF -f GZIP=4 command to reduce file size.</li> <li>EMD file can be processed with DIALS using <a href="https://github.com/keitaroyam/yamtbx/blob/master/dxtbx_formats/FormatEMD.py">this dxtbx format</a> file.</li> <li>Metadata (machine parameters, stage tilt angles etc.) is stored as json format in /Data/Image/*/Metadata in emd file. See <a href="https://github.com/keitaroyam/yamtbx/wiki/EMD-file">here</a> for details.</li> <li>If you want to process data using DIALS, please see <a href="https://github.com/keitaroyam/yamtbx/wiki/Processing-biotin-MicroED-data-(Krios-and-CetaD)">the processing note</a>.</li> </ul>
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>
Influence of Titan's Variable Electromagnetic Environment on the Global Distribution of Energetic Neutral Atoms
<p>Data for the manuscript "Influence of Titan's Variable Electromagnetic Environment on the Global Distribution of Energetic Neutral Atoms" by Tippens et al., (2022). See README.txt for a description of the data files included here.</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>
Dataset: Titan Pharmaceuticals, Inc. (TTNP) Stock Performance
This dataset provides historical stock market performance data for specific companies. It enables users to analyze and understand the past trends and fluctuations in stock prices over time. This information can be utilized for various purposes such as investment analysis, financial research, and market trend forecasting.
Dataset: Titan Machinery Inc. (TITN) Stock Performance
This dataset provides historical stock market performance data for specific companies. It enables users to analyze and understand the past trends and fluctuations in stock prices over time. This information can be utilized for various purposes such as investment analysis, financial research, and market trend forecasting.
Modeling the Emission of Energetic Neutral Atoms in Titan's Dynamic Magnetospheric Environment
<p>Data for the manuscript "Modeling the Emission of Energetic Neutral Atoms in Titan's Dynamic Magnetospheric Environment" by Tippens et al., (2024). See README.txt for a description of the data files included here.</p>
Rapid Impact Crater Relaxation Caused by An Insulating Methane Clathrate Crust on Titan: Data and Marc Files
<p><span>Data files for several figures in the manuscript "Rapid Impact Crater Relaxation Caused by An Insulating Methane Clathrate Crust on Titan" Published in The Planetary Science Journal. This includes data for the following figures: 4, 6, 7, 8 and 10. Two example Hexagon Marc-Mentat mud files for the axisymmetric thermal simulation and mechanical simulation of a 10 km thick clathrate, 85 km diameter crater are also included.</span></p> <p><span>Each column is self-explanatory except for the two relative depth data files. "Relative_Depth_Deep_Fig8" includes the results for simulations that use the initially deeper crater depth, and "Relative_Depth_Shallow_Fig8" includes the results for simulations that use the initially shallower crater depth. The columns are labeled with a shorthand notation for pairs of columns that represent the relative crater depth at specified times in the simulation. An example of time is “t(yr)_v21_120_5” and the corresponding relative depth column is “v21_Rd_120_5.” Time is given in years and relative depth is unitless. These specific examples provide results for a simulation that has a viscosity cutoff of 10^21 Pa s and a 120 km diameter crater with a 5 km thick methane clathrate crust overlying water ice.</span></p>
FIG. 1. — Comactinia titan n in Three new species of Comasteridae (Echinodermata, Crinoidea) from the tropical western Pacific
FIG. 1. — Comactinia titan n. sp.; A, B, P1 pinnule comb in aboral (A) and lateral (B) views (MNHN EcCh 185); C, cirrus (MNHN EcCh 186); D, cirrus (MNHN EcCs 10234); E, portion of centrodorsal and base of one ray (with abnormal br4+5 on right arm) (MNHN EcCh 186); F-H, pinnules (MNHN EcCh 186); F, P14; G, P5; H, P1. Scale bars: A, B, 1 mm; C-H, 5 mm.
Most rotifer species have positive responses in abundance caused by the increase in nitrogen, phosphorus and chlorophyll-a in reservoirs using TITAN analysis
<p>Some zooplanktonic species change their abundances according to the primary productivity increases in freshwater lentic environments. Here, we aimed to i) evaluate the concentration threshold of variables related to eutrophication (nitrogen, phosphorus<br> and chlorophyll-a concentrations) that alter the frequency of occurrence and relative abundance of rotifer species, and ii) analyze which Rotifera species are related positively or negatively to the increase in these variables. The rotifer community<br> structure was studied in fifteen reservoirs in La Plata River Basin, the second largest in South America, relating its abundance with nitrogen, phosphorus and chlorophyll-a values using the Threshold Indicator Rate Analysis (TITAN). Seventy-one rotifer<br> species were registered in the reservoirs, and six species were considered as indicators of changes in their frequency of occurrence and relative abundance with points of change of 1.118 µg.L -1 , 22.44 µg.L -1 and 3.89 µg.L -1 of the nitrogen, phosphorus and<br> chlorophyll-a concentrations, respectively. Species with positive responses to the increase in nutrients were Keratella tropica, Plationus patulus, Filinia terminalis and Synchaeta oblonga, and negative responses Conochilus unicornis and Synchaeta stylata,<br> typical of oligotrophic reservoirs. The only species that presented the same response for all variable concentrations was Keratella tropica, which is a very common species in South America. Our results reinforce the assumption that some rotifer species are good<br> indicators to the variables related to the trophic level in reservoirs. The script and study data are attached to this database.</p>
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OpenNeuro
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