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28 results for “Ganymede”
MHD Model of Ganymede's Magnetosphere: Predicted OCFB and magnetic footprint surface locations for Juno's flyby
<p>This dataset contains model results from a magnetohydrodynamic (MHD) model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021. Here we publish coordinates for the predicted location of the open-closed-field line-boundary (OCFB) on Ganymede's surface. Additionally we provide coordinates of Juno's magnetic footprint, namely the surface locations that connect to Juno's trajectory through magnetic field lines.</p> <p>For the surface locations we use a western longitude planetographic coordinate system where 0° longitude is in direction of the y-axis and 90° in direction of the x-axis of the cartesian GPhiO system. The GPhiO system is defined by the primary direction<br> z parallel to Jupiter’s rotation axis, the secondary direction y is pointing towards Jupiter barycenter<br> and x completes the right-handed system approximately in direction of plasma flow.</p> <p><strong>Duling2022_JunoGanymede_modeled_surface_OCFB.txt</strong></p> <p>Columns:</p> <p>Longitude [°]<br> Northern OCFB latitude [°]<br> Southern OCFB latitude [°]</p> <p><strong>Duling2022_JunoGanymede_modeled_magnetic_footprint.txt</strong></p> <p>Columns:</p> <p>Spacecraft time [UTC]<br> Magnetic footprint longitude [°]<br> Magnetic footprint latitude [°]<br> Length of field line between Juno and surface [radii]<br> Length of field line between Juno and surface [km]<br> r coordinate of Juno [radii]<br> Latitude of Juno [°]<br> Longitude of Juno [°]<br> x of Juno in GPhiO [km]<br> y of Juno in GPhiO [km]<br> z of Juno in GPhiO [km]</p> <p><strong>Duling2022_JunoGanymede_surface_map.png</strong></p> <p>A plot that visualizes the data of this repository.</p>
In situ observations of Ganymede's outflowing ionosphere
<p>The file contains values for ionospheric moments from the Juno flyby of Ganymede on 7 June 2021, during the period between 16:50 to 17:00, UTC. A description of the flyby and the data set is found in Valek et al. (2022), <em>In situ ion composition observations of the Ganynmede's outflowing ionosphere</em>, GRL DOI:10.1029/2022GL100281.</p>
MHD Model of Ganymede's Magnetosphere: Predicted magnetic field on Juno's trajectory
<p>This dataset contains model results from a magnetohydrodynamic (MHD) model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021. Here we publish predicted magnetic field components on Juno's trajectory that can be compared to MAG measurements and are displayed in Figure 3 of Duling et al. (2022).</p> <p>Each file contains data from one model. The dataset includes all models with parameter variations from Duling et al. (2022). These are summarized in Table 1 of Duling et al. (2022) and displayed in Figure 3 with the gray lines.</p> <p>If not varied, all models are run with the following parameters:</p> <p>Upstream Jovian background magnetic field B<sub>0 </sub>= (−15,24,−75) nT<br> Upstream plasma velocity v<sub>0</sub> = 140 km/s<br> Upstream plasma mass density <span class="math-tex">\(\rho\)</span><sub>0</sub> = 100 amu/cm<sup>3</sup><br> Upstream plasma thermal pressure p<sub>0</sub> = 2.8 nPa<br> Ionization frequency <span class="math-tex">\(\nu_{ion}\)</span> = 2.2e-8/s<br> Atmospheric surface mass density <span class="math-tex">\(n_{n,0}\)</span> = 8e6/cm<sup>3</sup><br> Dipole Gauss coefficient <span class="math-tex">\(g_1^0\)</span> = −716.8 nT</p> <p> </p> <p>The published data files correspond to the following models with each one parameter variation:</p> <table> <thead> <tr> <th scope="col">Parameter</th> <th scope="col">Value</th> <th scope="col">Filename Suffix</th> </tr> </thead> <tbody> <tr> <td>default model</td> <td> - </td> <td>default</td> </tr> <tr> <td>Upstream Jovian background magnetic field (measured before flyby)</td> <td>B<sub>0 </sub>= (−16,3,−70) nT</td> <td>B0before</td> </tr> <tr> <td>Upstream Jovian background magnetic field (measured after flyby)</td> <td>B<sub>0 </sub>= (−14,43,−80) nT</td> <td>B0after</td> </tr> <tr> <td>Upstream plasma velocity (min)</td> <td>v<sub>0</sub> = 120 km/s</td> <td>v-</td> </tr> <tr> <td>Upstream plasma velocity (max)</td> <td>v<sub>0</sub> = 160 km/s</td> <td>v+</td> </tr> <tr> <td>Upstream plasma mass density (min)</td> <td><span class="math-tex">\(\rho\)</span><sub>0</sub> = 10 amu/cm<sup>3</sup></td> <td>rho-</td> </tr> <tr> <td>Upstream plasma mass density (max)</td> <td><span class="math-tex">\(\rho\)</span><sub>0</sub> = 160 amu/cm<sup>3</sup></td> <td>rho+</td> </tr> <tr> <td>Upstream plasma thermal pressure (min)</td> <td>p<sub>0</sub> = 1.0 nPa</td> <td>p-</td> </tr> <tr> <td>Upstream plasma thermal pressure (max)</td> <td>p<sub>0</sub> = 5.0 nPa</td> <td>p+</td> </tr> <tr> <td>Ionization frequency (min)</td> <td> <span class="math-tex">\(\nu_{ion}\)</span> = 0.5e-8/s</td> <td>prod-</td> </tr> <tr> <td>Ionization frequency (max)</td> <td> <span class="math-tex">\(\nu_{ion}\)</span> = 10.0e-8/s</td> <td>prod+</td> </tr> <tr> <td>Atmospheric surface mass density (min)</td> <td> <span class="math-tex">\(n_{n,0}\)</span> = 1.6e6/cm<sup>3</sup></td> <td>nn-</td> </tr> <tr> <td>Atmospheric surface mass density (max)</td> <td> <span class="math-tex">\(n_{n,0}\)</span> = 40e6/cm<sup>3</sup></td> <td>nn+</td> </tr> <tr> <td>Dipole Gauss coefficient (min)</td> <td> <span class="math-tex">\(g_1^0\)</span> = −702.5 nT</td> <td>dipole-</td> </tr> <tr> <td>Dipole Gauss coefficient (max)</td> <td> <span class="math-tex">\(g_1^0\)</span> = −731.1 nT</td> <td>dipole+</td> </tr> </tbody> </table> <p>Magnetic Field components and Juno's position are in GPhiO system. GPhiO is defined by the primary direction z parallel to Jupiter’s rotation axis, the secondary direction y is pointing from Ganymede's towards Jupiter's barycenter and x completes the right-handed system approximately in direction of plasma flow.</p> <p>Columns:</p> <p>Spacecraft time [UTC]<br> Bx modeled magnetic field in GPhiO [nT]<br> By modeled magnetic field in GPhiO [nT]<br> Bz modeled magnetic field in GPhiO [nT]<br> B modeled magnetic field magnitude [nT]<br> x of Juno in GPhiO [km]<br> y of Juno in GPhiO [km]<br> z of Juno in GPhiO [km]</p>
Control Network for Ganymede Images from JunoCam Perijove 34
<p>Delivered is a photogrammetric control network for four images of Ganymede collected by the Juno- Cam instrument during the Juno mission’s perijove 34 encounter on 2021-06-07. The network has 184,659 control points and 369,318 control measures (2 measures per control point). The network is a PVL formatted text file for use in ISIS (Integrated Software for Imagers and Spectrometers). When control points are merged with an image distance tolerance of 1.0 pixel the resulting network has 83,096 control points and 233,598 control measures. Extracting control points with 4 or more measures yields a network with 16,709 control points and 75,197 control measures.</p> <p>The initial network is produced with novel code implemented in Mathematica.</p> <p>In the “Initial Network” 98% of residuals are less than 1.72 pixels. Median residual is .40 pixels. There are 54 control points with residuals greater than 3 pixels, and 1544 with greater than 2.</p> <p>See ControlNetworkJunoCamV16j.pdf for details.</p>
Corresponding Dataset for "Ganymede's Ionosphere observed by a Dual-Frequency Radio Occultation with Juno"
<p> Corresponding Dataset for "Ganymede’s Ionosphere observed <br> by a Dual-Frequency Radio Occultation with Juno"<br> README FILE<br> VERSION 2<br> Dustin Buccino<br> April 22, 2024<br> Jet Propulsion Laboratory<br> California Institute of Technology</p> <p>=============================================================================<br>VERSION 2 INFORMATION<br>=============================================================================</p> <p> Version 2 of this dataset separates the Electron Density profile from the<br>main data files and makes a correction to the egress profile that was<br>discovered. Differences in egress profile are very small and within<br>the uncertainties. Furthermore egress is statistically a non-detection<br>(zero densities), but for sake of accuracy they are reposted to be<br>consistent with the publication.</p> <p>=============================================================================<br>INTRODUCTION<br>=============================================================================</p> <p> This dataset contains processed radio science data and results of the<br>Juno Ganymede radio occultation. This dataset is provided in order to <br>supplement the submitted article to the "Geophysical Research Letters"<br>journal:</p> <p> Buccino, D.R., et al (2022), Ganymede’s Ionosphere observed by a <br> Dual-Frequency Radio Occultation with Juno, Geophysical Research <br> Letters, submitted February 2022.</p> <p><br> Please note the raw data used in this analysis are not provided in this<br>supplementary dataset. The raw Juno Gravity Science Data may be found at <br>the Planetary Data System:</p> <p> Buccino, D. R. (2016). Juno jupiter gravity science raw data set <br> V1.0, JUNO-J-RSS-1 JUGR-V1.0, NASA planetary data system (PDS). <br> Retrieved from https://atmos.nmsu.edu/PDS/data/jnogrv_1001/<br> </p> <p>=============================================================================<br>ARCHIVE INFORMATION<br>=============================================================================</p> <p> This archive contains two files within the root directory.<br> <br> ROOT<br> `- JunoG34OccData_Egress_v2.csv</p> <p> This data file contains the EGRESS data relevant to the radio<br> occultation. The data is a timeseries of impact parameter, sky<br> sky frequency at X-band and Ka-band, the dual-frequency <br> combination, the calibrated dual-frequency, Total Electron <br> Content.</p> <p> `- JunoG34_GRL_Egress_Profile_v2.csv</p> <p> This data file contains the EGRESS Electron density, and <br> 1-sigma electron density uncertainty.</p> <p> `- JunoG34OccData_Ingress_v2.csv</p> <p> This data file contains the INGRESS data relevant to the radio<br> occultation. The data is a timeseries of impact parameter, sky<br> sky frequency at X-band and Ka-band, the dual-frequency <br> combination, the calibrated dual-frequency, Total Electron <br> Content.</p> <p> `- JunoG34_GRL_Ingress_Profile_v2.csv</p> <p> This data file contains the INGRESS Electron density, and <br> 1-sigma electron density uncertainty.</p> <p>=============================================================================<br>FILE FORMAT<br>=============================================================================</p> <p> This dataset contains only a comma-separated text files which are<br>given with the "*.csv" extension.</p> <p><br> CSV FILES<br> -------------------------------------------------------------------------</p> <p> The Comma-Separated Value (CSV) files are plain-text files. Values in<br> each data file are separated using a comma ",". Each column is defined <br> by a header row which provides a description of each column.<br> </p> <p>=============================================================================<br>ACKNOWLEDGMENTS<br>=============================================================================</p> <p>This work was carried out at the Jet Propulsion Laboratory, <br>California Institute of Technology, under contract with the National <br>Aeronautics and Space Administration. Government sponsorship acknowledged.</p> <p>EG, LGC, PT, MZ and AC are grateful to the Italian Space Agency (ASI) for <br>financial support through Agreement No. 2018-25-HH.0 in the context of ESA's <br>JUICE mission, and Agreement No. 2017-40-H.1-2020, and its extension <br>2017-40-H.02020-13-HH.0, for ESA’s BepiColombo and NASAs Juno radio science <br>experiments. EG is grateful to "Fondazione Cassa dei Risparmi di Forlì" for <br>financial support of his PhD fellowship.</p> <p>PS and AH were supported by NASA Contract NNM06AA75C from the Marshall <br>Space Flight Center under subcontract 699054X from Southwest Research <br>Institute.</p> <p><br>=============================================================================<br>PRIMARY POINT OF CONTACT<br>=============================================================================</p> <p>Dustin Buccino<br>Jet Propulsion Laboratory<br>Planetary Radar and Radio Sciences<br>(818) 393 - 1072<br>Dustin.R.Buccino@jpl.nasa.gov</p> <p>=============================================================================<br>ACRONYMS AND ABBREVIATIONS<br>=============================================================================</p> <p> ASCII American Standard Code for Information Interchange<br> DOY Day of year<br> DSN Deep Space Network<br> JPL Jet Propulsion Laboratory<br> NAIF Navigation Ancillary Information Facility<br> NASA National Aeronautics and Space Administration<br> PDS Planetary Data System<br> RS Radio Science<br> RSS Radio Science Subsystem<br> SIS Software Interface Specification<br> TXT Text file<br> UTC Universal Time, Coordinated</p>
Data for the research article: "Simulations of Energetic Neutral Atom sputtering from Ganymede in preparation for the JUICE mission"
<p>Data for the research article: "Simulations of Energetic Neutral Atom sputtering from Ganymede in preparation for the JUICE mission"</p>
Corresponding Dataset for Gravity Field of Ganymede after the Juno Extended Mission
<p>Corresponding Dataset for Gravity Field of Ganymede after the Juno Extended Mission</p> <p> Luis Gomez Casajus August 2, 2022</p> <p>=============================================================================<br> Introduction<br> =============================================================================</p> <p> This dataset contains the estimated gravity field and its corresponding<br> full covariance matrix. This dataset is provided in order to <br> supplement the submitted article to the "Geophysical Research Letters"<br> journal:</p> <p> Gravity Field of Ganymede after the Juno Extended Mission.<br> L. Gomez Casajus (*), A. I. Ermakov, M. Zannoni, J. T. Keane, <br> D. Stevenson, D. R.Buccino, D. Durante, M. Parisi, R. S. Park, <br> P. Tortora and S. J. Bolton<br> <br> - (*) luis.gomezcasajus@unibo.it</p> <p>=============================================================================<br> File description<br> =============================================================================</p> <p> This archive contains two files within the root directory.<br> <br> ROOT<br> -SOI_gravity_field.txt</p> <p> This file contains the estimated normalized spherical harmonics <br> coefficients of the Ganymede gravity field.<br> The file contains a header row which provides a description of <br> the file.</p> <p> -SOI_cov_matrix.txt</p> <p> This file contains the estimated full covariance matrix (32x32) <br> of the normalized spherical harmonics coefficients of the <br> Ganymede gravity field. The file contains a header row which <br> provides a description of the file. The matrix is represented as<br> a 2 dimensional array whose coefficients follow the following <br> order scheme: C20 C21 S21 C22 S22 C30 C31 ...</p> <p>=============================================================================<br> ACKNOWLEDGMENTS<br> =============================================================================</p> <p> The authors are grateful to William Folkner, to the entire Solar System <br> Dynamics Group and to Robert Haw, former Galileo navigator, for the useful <br> discussions and suggestions regarding the procedures for Galileo data <br> analysis. L.G.C., M.Z., and P.T. are grateful to the Italian Space Agency <br> (ASI) for financial support through Agreement No. 2017-40-H.1-2020, and its <br> extension2017-40-H.02020-13-HH.0, for ESA’s BepiColombo and NASA’s Juno radio<br> science experiments. L.G.C., M.Z., and P.T. acknowledge Caltech and the Jet <br> Propulsion Laboratory for granting the University of Bologna a license to an <br> executable version of MONTE Project Edition S/W. JTK and AIE acknowledge <br> support from the Juno participating scientist program. The work of RP, DB, <br> JTK, and MP was carried out at the Jet Propulsion Lab, California Institute<br> of Technology, under a contract with the National Aeronautics and Space <br> Administration (80NM0018D0004). Government sponsorship acknowledged. </p>
MHD model output for Ganymede's magnetosphere during Juno's flyby
<p>This dataset contains the complete simulation output from our MHD model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021 (Duling et al. 2022).</p> <p>The data was obtained by our application of the PLUTO simulation code v4.4 (Mignone et al. 2007) (http://plutocode.ph.unito.it/) described in Duling et al. 2022.</p> <p>The dataset includes the simulation variables on the simulation grid for a single timestep after steady state was reached. The grid has spherical geometry (r, theta, phi) with phi=0° longitude pointing towards Jupiter (positive y axis of the GPhiO system), phi=90° longitude pointing in the upstream direction (negative x axis of GPhiO) and theta=0° latitude at Ganymede's north pole (positive z axis of GPhiO). The following model variables are included:</p> <p>rho: plasma mass density<br> prs: thermal plasma pressure<br> vx1: plasma velocity radial component<br> vx2: plasma velocity theta component<br> vx3: plasma velocity phi component<br> Bx1: magnetic field radial component<br> Bx2: magnetic field theta component<br> Bx3: magnetic field phi component</p> <p>Additionally the following derived variables are included:</p> <p>Jx1: electric current density radial component<br> Jx2: electric current density theta component<br> Jx3: electric current density phi component<br> Bpx1: plasma magnetic field radial component<br> Bpx2: plasma magnetic field theta component<br> Bpx3: plasma magnetic field phi component</p> <p>Plasma magnetic field means that part of the total magnetic field that results from the plasma interaction. It equals the total magnetic field subtracted by the homogeneous upstream field and Ganymede's intrinsic and induced field.</p> <p>All values are in normalized units with these normalization factors:</p> <p>NORMR = 2.631e8 cm<br> NORMV = 1.4e7 cm/s<br> NORMRHO = 1.661e-22 g/cm^3<br> NORMPRS = 3.255e-08 dyne/cm^2<br> NORMB = 6.395e-04 Gauss<br> NORMJ = 5.801e-03 statA/cm^2</p> <p>In Duling et al. 2022 we present results of a model sensitivity study. This dataset includes model output from our best guess setup (default setup) only.</p> <p>Since the data is in PLUTO's binary format "flt" we provide a Python code snippet that reads the data to data arrays.</p> <p><strong>grid.out</strong><br> This ASCII file contains the grid dimensions and coordinates of the cell boundaries.</p> <p><strong>data.0020.flt</strong><br> This binary file contains the simulation variables on the cell centers of the grid.</p> <p><strong>pluto.0.log</strong><br> This ASCII file contains the header of the PLUTO logfile.</p> <p><strong>read_data.py</strong><br> This Python code snippet helps with reading the data.</p>
Supporting data for "The high-frequency tidal response of ocean worlds: Application to Europa and Ganymede"
<p>Data files containing the static Love numbers that are used to compute the dynamic Love numbers.</p> <p> </p>
Juno Stellar Reference Unit (SRU) image data from Juno's G34 Ganymede flyby on 7 June 2021
<p>This is the Juno Stellar Reference Unit (SRU) image data from Juno's G34 Ganymede flyby on 7 June 2021. The image is discussed in the paper, "Surface features of Ganymede revealed in Jupiter-shine by Juno's Stellar Reference Unit," published in AGU Geophysical Research Letters.</p>
Electron Physics in 3D Two-Fluid Ten-Moment Modeling of Ganymede's Magnetosphere
<p>The dataset is produced for the manuscript "Electron Physics in 3D Two-Fluid Ten-Moment Modeling of Ganymede's Magnetosphere" accepted by the JGR - Space Physics. The script mirdip.lua was used to perform the simulation by the Gkeyll multi-fluid high-moment code. The simulation produced output files in the HDF5 format following the VizSchema description, both are open-source. The output file can be visualized by free, open-source toolkit ParaView. In the file mirdip_q_10.h5, the state quantities are stored in the 4d array "StructGridField" in the layout of NZ * NY * NX * NCOMP, where NX, NY, and NZ are cell numbers in each direction, and NCOMP = 28 is the number of state quantities in the order of ten electron moment terms, ten ion moment terms, six electromagnetic field terms and two correction potential terms.</p>
Energetic Electron Lensing Caused by 375 Ganymede's Magnetic Field
<p>Suplementary meterial for the paper <em>Energetic Electron Lensing Caused by Ganymede’s Magnetic Field</em> (perijove radiation data).</p>
Spherical harmonic model of the gravitational potential of Ganymede from Gomez Casajus et al. (2022)
<p>Ganymede2022 is a spherical harmonic model of the gravitational potential of Ganymede that makes use of data from Galileo and the JUNO extended mission. The data in the file Ganymede2022.sh.gz are identical to those in the submission <a href="../record/6949645">6949645</a> (Gomez Casajus et al. 2022) with the exception that they have been reformatted in a way that facilitates their reading by the python package pyshtools, and the GM has been included (personal communication from the original authors).</p>
Dataset for "Microwave Observations of Ganymede's Sub-Surface Ice Part II: Reflected Radiation"
<p>Dataset for figures in paper "Microwave Observations of Ganymede's Sub-Surface Ice Part II: Reflected Radiation".</p>
Attis (or Ganymedes)
Attis (or Ganymedes), bust, wearing Phrygian cap Find Spot: source not stated Material: marble (Luna) Dimension: height, 0.398, m Acquisition: given; 1850; Disney, John, Dr Documentation: Michaelis, Adolf. 1882. Ancient marbles in Great Britain. no. 44 Budde, Ludwig. Nicholls, Richard V.. 1967. Catalogue of the Greek and Roman sculpture in the Fitzwilliam Museum, Cambridge. no. 54, pl. 16 Brussels. Credit Communal. Marbres helleniques de la carriere au chef d'oeuvre. 172 no.113 Disney, J.. 1846. Museum Disneianum : being a description of a collection of ancient marbles, in the possession of John Disney. pl. vi 1968. [Unknown: Art Bulletin September 1968]. Source Title: Art Bulletin(September-) Object Number: GR.13.1850 (Antiquities) https://data.fitzmuseum.cam.ac.uk/id/object/65482 Source: Objaverse 1.0 / Sketchfab
HIV Acquisition and Life Course of Born-abroad Men Who Have Sex With Men Living in Ile-de-France: the GANYMEDE Study
ClinicalTrials.gov study NCT04684758. IPD Sharing: NO. Countries: 1. Publications: 0.
Thermal and energetic ion dynamics in Ganymede's magnetosphere
Open the record for dataset details and reuse information.
Repository - Ganymede's far-ultraviolet reflectance: constraining impurities in the surface ice
<p>This repository contains the modeled spectra and material optical properties used to produce Figures 3-11 in the main text, and the supplementary figures.</p>
Inner Core Composition of the Moon and Ganymede revealed by Thermal Equation of State of Fe0.99C0.01 alloy
Open the record for dataset details and reuse information.
Dataset:Ray and Halo impact craters on Ganymede : fingerprint for decoding Ganymede´s crustal structure
<p>The geological basemap used in the study is from Kersten et al., 2021. </p>
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