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17 results for “Venus Express”
Predicted times of bow Shock crossings at Venus from the ESA/Venus Express mission, using spacecraft ephemerides and magnetic field data, with a predictor-corrector algorithm
<p><strong>CHARACTERISTICS</strong><br> Planet: <strong>Venus</strong><br> Radius: <strong>R<sub>V</sub> = 6051.8 km</strong> (volumetric mean planetary radius)<br> Spacecraft: <strong>ESA/Venus Express</strong><br> Spacecraft coordinates system: <strong>Venus Solar Orbital (VSO)</strong> equivalent to <em>Sun-State </em>coordinate system:</p> <ul> <li>+<em>X<sub>VSO</sub></em> points towards the Sun from the planet’s centre,</li> <li>+<em>Z<sub>VSO</sub></em> towards Venus’ North pole and perpendicular to the orbital plane defined as the <em>X<sub>VSO</sub></em>–<em>Y<sub>VSO</sub></em> plane passing through the centre of Venus,</li> <li><em>Y<sub>VSO</sub></em> completes the orthogonal system.</li> </ul> <p>Time span: <strong>01/04/2006 to 25/11/2014</strong><br> Total number N of candidate bow shock crossings in the database: <strong>N = 4950</strong><br> Number of quasi-parallel bow shock crossings: <strong>N<sub>||</sub> = 844</strong><br> Number of quasi-perpendicular bow shock crossings: <strong>N<sub><span class="math-tex">\(\perp\)</span></sub> = 4106</strong></p> <p><strong>ORIGINAL DATASETS USED</strong><br> The original Venus Express/MAG data repository on which these algorithms were applied is available on ESA's Planetary Science Archive system (PSA) at: https://archives.esac.esa.int/psa/ftp/VENUS-EXPRESS/MAG/. For this study, 1-Hz magnetic field data was used.</p> <p><strong>METHOD</strong><br> To construct this database from the original datasets above, the predictor and predictor-corrector algorithms used are described for the Mars case in:<br> Simon Wedlund, C., Volwerk, M., Beth, A., Mazelle, C., Möstl, C., Halekas, J., Gruesbeck, J. and Rojas-Castillo, D., (2021), A Fast Bow Shock Location Predictor-Estimator From 2D and 3D Analytical Models: Application to Mars and the MAVEN mission, <em>Journal of Geophysical Research</em>, <strong>127</strong>, e2021JA029942. <a href="https://doi.org/10.1029/2021JA029942">https://doi.org/10.1029/2021JA029942</a></p> <p>They consist of two consecutive steps: </p> <ol> <li>Predictor geometric algorithm based on 2D or 3D existing fits for prediction of the Venus bow shock position. The original fits were taken from 2D conic fits in the plane <span class="math-tex">\(\left(X_\text{VSO}, \sqrt{Y_\text{VSO}^2+Z_\text{VSO}^2}\right)\)</span>performed on the datasets of <strong>Persson et al. (2023)</strong>, Venusian bow shock crossings manually identified from measurements by the ASPERA-4 and MAG instruments onboard Venus Express, <em>Zenodo</em> (<a href="http://doi.org/10.5281/zenodo.7679677">https://doi.org/10.5281/zenodo.7679677</a>).</li> <li>Corrector algorithm based on magnetic field measurements.</li> </ol> <p>We also provide the angle between the average Interplanetary Magnetic Field (IMF) vector upstream of the shock and the shock normal, noted <span class="math-tex"><em>θ</em><sub><em>B</em><em>n</em></sub></span> (ThetaBn). Assuming a locally smooth shock surface, this gives a first indication of the geometry of the shock, so that:</p> <ul> <li><span class="math-tex">45<sup>∘</sup><<em>θ</em><sub><em>B</em><em>n</em></sub><135<sup>∘</sup></span>: quasi-perpendicular shock condition</li> <li><span class="math-tex"><em>θ</em><sub><em>B</em><em>n</em></sub>≤45<sup>∘</sup> and <em>θ</em><sub><em>B</em><em>n</em></sub><span class="math-tex">\(\geq\)</span>135<sup>∘</sup></span>: quasi-parallel shock condition</li> </ul> <p>Uncertainty on these angles is estimated to be ± 5º. </p> <p>For details, see <strong>Simon Wedlund et al. (2022)</strong> above, §2.3 pp. 10-12.</p> <p><strong>VARIABLES DESCRIPTION</strong></p> <p>This database contains the following ASCII variables:</p> <ul> <li>Bow shock times in Venus Express' database (1-s resolution): <em>T</em><sub>bs</sub></li> <li>Venus Solar Orbital coordinates of the shock, in units of Venus radius <em>R</em><sub>V </sub>(<em>R</em><sub>V</sub> = 6051.8 km):<br> <em>X<sub>VSO</sub></em>,<sub> </sub><em>Y<sub>VSO</sub></em>, <em>Z<sub>VSO</sub></em> and Euclidean distance <span class="math-tex">\(R_{VSO} = \sqrt{X_{VSO}^2 + Y_{VSO}^2 + Z_{VSO}^2}\)</span> (in <em>R<sub>V</sub></em>)</li> <li>Solar Zenith angle in degrees: <em>SZA</em> = <span class="math-tex">\(\tan^{-1}{Y_{VSO}^2+Z_{VSO}^2 \over X_{VSO}^2}\)</span> (in º) </li> <li>Angle between average B-field direction and shock normal assuming a smooth shock surface <span class="math-tex">\(\theta_{Bn}\)</span> (ThetaBn, in º, calculated with atan2(norm(cross(<strong>B</strong>,<strong>ñ</strong>),dot(<strong>B</strong>,<strong>ñ</strong>)), with <strong>B</strong> the magnetic field vector and <strong>ñ</strong> the vector normal to the shock surface): <ul> <li>45 < ThetaBn < 135 deg: quasi-<span class="math-tex">\(\perp\)</span> shock</li> <li>ThetaBn <span class="math-tex">\(\leq\)</span> 45 deg & ThetaBn <span class="math-tex">\(\geq\)</span> 135 deg: quasi-|| shock</li> </ul> </li> <li>Interplanetary Magnetic Field (IMF) upstream average vector in VSO coordinates, <em>B<sub>x</sub></em>, <em>B<sub>y</sub></em>, <em>B<sub>z</sub></em> (in nT).</li> <li>Flag for direction of crossing: <ul> <li>flag = 0: magnetosheath <span class="math-tex">\(\longrightarrow\)</span> solar wind (2447 events)</li> <li>flag = 1: solar wind <span class="math-tex">\(\longrightarrow\)</span> magnetosheath (2503 events)</li> </ul> </li> </ul> <p><strong>WARNING</strong></p> <ol> <li>This version of the database is currently in a preliminary stage of application and, as such, is not fully tested. Solar wind upstream magnetic field values (IMF) are given only as a first approximation for each orbit segment. See point 2 for caveats. For carefully manually picked shock crossings, the user is referred to the database of:<br> <strong>Persson et al. (2023)</strong>, Venusian bow shock crossings manually identified from measurements by the ASPERA-4 and MAG instruments onboard Venus Express, <em>Zenodo</em> (<a href="http://doi.org/10.5281/zenodo.7679677">https://doi.org/10.5281/zenodo.7679677</a>)</li> <li>This database is based on an automatic statistical geometrical estimate, further refined by constraints on magnetic fields. This is aimed at giving a first approximation of the shock area times in the Venus Express data. It is particularly suited to statistical studies and region identification in the Venus Express datasets. As such, this database should be used as a <em>first indicator</em> of the shock location, and <em>with</em> <em>caution</em>: it <strong>CANNOT</strong>, and <strong>WILL NOT </strong>substitute, especially in case studies, for a careful analysis of the full magnetometer and plasma bow shock signatures. Moreover, the algorithm is optimised for detecting the first disturbance observed in the magnetic field immediately ahead of the shock's foot (in the foreshock area), and not for the detection of other structures in the shock, such as the shock ramp. The "shock" location is therefore given here with typical uncertainties of about 0.040 R<sub>V</sub> (with R<sub>V</sub> = 6051.8 km, i.e., about 250 km in the radial direction). Finally, for multiple shock crossings, the algorithm chooses the first occurrence of the shock starting from the undisturbed solar wind.</li> </ol> <p>Current formatting optimised for MATLAB.</p> <p><strong>ACKNOWLEDGEMENTS</strong><br> C. Simon Wedlund and M. Volwerk thank the Austrian Science Fund (FWF) project P32035-N36. </p> <p><strong>LICENSE AND RIGHTS</strong><br> This database is shared under a Creative Commons CC-BY-4.0 license.</p> <p>Version 1 (c) Cyril Simon Wedlund @ Space Research Institute of Graz (IWF), <br> Austrian Academy of Sciences, 2022-10-05<br> Contact email: cyril.simon.wedlund@gmail.com</p>
[Dataset] Spatial and temporal variability of the 365-nm albedo of Venus observed by the camera on board Venus Express
<p>This is the derived data, presented in a publication entitled "Spatial and temporal variability of the 365-nm albedo of Venus observed by the camera on board Venus Express" (JGR:Planet, doi: 10.1029/2019JE006271). See the paper for details. See 'Readme.txt' for the file descriptions.</p>
Venusian bow shock crossings manually identified from measurements by the ASPERA-4 and MAG instruments onboard Venus Express
<p>Bow shock crossings at Venus identified manually from the ASPERA-4 and MAG instruments onboard Venus Express for the full mission from 2006 to 2014.</p> <p>A detailed description of the dataset can be found in the paper "Influence of solar wind variations on the shapes of Venus’ plasma boundaries based on Venus Express observations" by Signoles et al.</p> <p>The boundary crossings by Venus Express are determined from combining the measurements of both ion, electron and magnetic field measurements. The bow shock is identified from the sharp increase in the magnetic field magnitude, and the increase in electron and ion temperature. The ion composition boundary is identified from the decrease in magnetosheath protons and electrons, and the appearance of planetary heavy ions.</p> <p>The dataset contains 5193 identified bow shock crossings and 2679 identified ion composition boundary crossings.</p> <p>For more information on the dataset contact: M. Persson, moaperssonphd at gmail.com</p>
Fine vertical structures at the cloud heights of Venus revealed by radio holographic analysis of Venus Express and Akatsuki radio occultation data -- dataset
<p>The data used in the figures in the paper "Fine vertical structures at the cloud heights of Venus revealed by radio holographic analysis of Venus Express and Akatsuki radio occultation data" by Imamura et al. (J. Geophys. Res)</p> <p>The description of the columns in the files are given in the header section.</p>
The identified bow shock crossings based on Venus Express observations
<div>Bow shock locations and upstream parameters observed by Venus Express.</div> <div> </div> <div>The columns are structured as follows:</div> <div> 1: time of bow shock crossings dd-mmm-yyyy HH:MM:SS</div> <div> 2: X-VSE [Rv]</div> <div> 3: Y-VSE [Rv]</div> <div> 4: Z-VSE [Rv]</div> <div>5: Solar wind magnetosonic Mach number</div> <div> 6: EUV [mW/m^2]</div> <div> 7: IMF Bx in VSE [nT]</div> <div>8: IMF By in VSE [nT]</div> <div> 9: IMF intensity |B| [nT]</div> <div> 10: IMF cone angle [degree]</div> <div>11: Solar wind dynamic pressure [nPa]</div> <div>12: The angle between the IMF and the shock normal, thetaBn [degree]</div> <div> </div> <div>Please contact xuqi01@nssc.ac.cn if you have questions.</div>
Venus Express IMA solar wind data for VeRa radio science observations
<p>The Venus Express (VEX) Analyser of Space Plasmas and Energetic Atoms (ASPERA-4)<br>ion mass spectrometer (IMA) observed the the pristine solar wind parameters<br>at Venus between 2006 and 2014. Details can be found in<br>Barabash et al. (2007) Planetary and Space Science, Vol. 55 (12), pp. 1772-1792<br>The Analyser of Space Plasmas and Energetic Atoms (ASPERA-4) for the <br>Venus Express mission.</p> <p>This file is based on the VEX_IMA_SW_NVP_20060101.cef data file provided<br>by M. Fränz (MPI for Solar System Research, Goettingen, Germany) and contains only those ASPERA-4<br>solar wind observations used in the publication Peter et al. (2024) Icarus<br>The variability of the topside ionospheres of Venus and Mars<br>as seen by recent radio science observations (Appendix A4 Fig. 2).</p> <p>Data are based on hourly average IMA spectra obtained when VEX was at larger distance than<br>1 Venus radius from nominal bow shock (Martinecz 2009, PhD). Density and total velocity<br>are obtained by integration over the IMA_EXTRA proton spectrum. Dynamic pressure<br>by product of density and velocity. This file contains only orbits used for VERA analyis.</p>
Vertical temperature profiles obtained from Venus Express and Akatsuki radio occultation data using FSI
<p>Vertical temperature profiles of Venusian atmosphere obtained from selected radio occultation data taken in ESA's Venus Express and JAXA's Akatsuki missions. The temperatures were retrieved using a radio holographic method, Full Spectrum Inversion (FSI). The data list and format are given in two Excel files and the data are given in text files with an extension ".dat".</p>
Cloud motion vectors used in "Formation of the Y feature at the Venusian cloud top by planetary-scale waves and the mean circulation: analysis of Venus Express VMC images"
<p>This is dataset of cloud motion vectors deduced used in "Formation of the Y feature at the Venusian cloud top by planetary-scale waves and the mean circulation: analysis of Venus Express VMC images".</p>
VENUS: Septic Gene Expression Using SeptiCyte
ClinicalTrials.gov study NCT02127502. IPD Sharing: NO. Countries: 1. Publications: 2.
Example measurements of electron energy and pitch angle distributions from Venus Express
Open the record for dataset details and reuse information.
Expression data from epidermal stem cells isolated from dorsal skin of P19 Per1-Venus mice and Bmal1 epidermal knockout mice
GEO Series GSE27079. Mus musculus. 12 samples. Type: Expression profiling by array.
Genes differentially expressed between NEUROG3-Venus positive and negative hiPSC line differentiated to pancreatic endocrine progenitors [RNA-Seq]
GEO Series GSE179261. Homo sapiens. 8 samples. Type: Expression profiling by high throughput sequencing.
VENUS EXPRESS SPICE KERNELS V2.0
This data set includes the complete set of Venus Express mission SPICE data files (``kernel files''), which can be accessed using SPICE software. The SPICE data contains geometric and other ancillary information needed to recover the full value of the science instrument data. In particular SPICE kernels provide spacecraft and planetary ephemerides, instrument mounting alignments, spacecraft orientation, spacecraft sequences of events, and data needed for relevant time conversions.
VENUS EXPRESS SPICE KERNELS V1.0
SPICE deals with ancillary data needed to support the planning for, and analysis of, science instrument data. As well as software (the SPICE toolkit) and documentation, SPICE provides data files, called kernels, that contain ancillary information which has been created in such a way as to allow easy access and correct usage by the space science and engineering communities.
Gene expression difference in cells expressing high and low FoxA2-Venus protein levels from mouse neural tube organoids.
GEO Series GSE221187. Mus musculus. 9 samples. Type: Expression profiling by high throughput sequencing.
VENUS EXPRESS SPICE KERNELS V1.0
SPICE deals with ancillary data needed to support the planning for, and analysis of, science instrument data. As well as software (the SPICE toolkit) and documentation, SPICE provides data files, called kernels, that contain ancillary information which has been created in such a way as to allow easy access and correct usage by the space science and engineering communities.
PDS Venus Express Radio Science Data Release
RSS
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