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430 results for “Jupiter”
Data for "Investigating temporary capture in the Sun-Jupiter three-body system via Lagrangian coherent structures"
<p>The supplementary online materials for the paper "Investigating temporary capture in the Sun-Jupiter three-body system via Lagrangian coherent structures" consist of two parts.</p> <h3>Part 1: Coordinates of the LCS Surfaces in Figure 8</h3> <p>This part contains the coordinates of the local maxima of FTLE (Finite-Time Lyapunov Exponent) values that compose the Lagrangian Coherent Structures (LCS) surface presented in Figure 8 of the paper. These coordinates are crucial for understanding the formation and characteristics of the LCS in the three-body system.</p> <h3>Part 2: Orbital States of Asteroid 2002 GV28 Based on the High-Fidelity Ephemeris Model from Section 2.2 of the Paper</h3> <p>This part includes the orbital states of asteroid 2002 GV28, propagated using a high-fidelity ephemeris model as described in Section 2.2 of the paper. The data provides information on the asteroid's state in two different coordinate systems:</p> <ol> <li> <p><strong>Heliocentric J2000.0 Ecliptic Coordinate System:</strong></p> <ul> <li>This dataset includes the position and velocity of the asteroid relative to the Sun at various time steps.</li> <li>The columns typically include: Time (Julian Date), X (km), Y (km), Z (km), Vx (km/s), Vy (km/s), Vz (km/s).</li> </ul> </li> <li> <p><strong>Sun-Jupiter Rotating Coordinate System:</strong></p> <ul> <li>This dataset provides the position and velocity of the asteroid relative to the Sun-Jupiter rotating frame.</li> <li>The columns typically include: Time (Julian Date), X (normlized), Y (normlized), Z (normlized), Vx (normlized), Vy (normlized), Vz (normlized).</li> </ul> </li> </ol> <p>Each entry in these datasets corresponds to specific time steps during the propagation, providing a comprehensive view of the asteroid's trajectory in both coordinate systems.</p>
Smoothed VLT/MUSE observations of Jupiter and Saturn
<p>Data are those used for the JGR submission: "Clouds and ammonia in the atmospheres of Jupiter and Saturn determined from a band-depth analysis of VLT/MUSE observations". Observation dates are 23rd March 2020 for Jupiter, and 6th April 2017 for Saturn.</p>
Derived data for: "Magnetic reconnection near the planet as a possible driver of Jupiter's mysterious polar auroras"
<p>Derived data for "Magnetic reconnection near the planet as a possible driver of Jupiter’s mysterious polar auroras", accepted for publication in the Journal of Geophysical Research: Space Physics.</p>
Data for Statistics on Jupiter's Current Sheet with Juno Data: Geometry, Magnetic Fields and Energetic Particles
<p>The statistical data of paper "Statistics on Jupiter’s Current Sheet with Juno Data: Geometry, Magnetic Fields and Energetic Particles"</p>
Warm Jupiter Flux Maps
<p>Gif and mp4 animations showing maps of the bolometric thermal emission from 3D atmospheric models of a hypothetical warm Jupiter, throughout one orbit (i.e., year) of the planet. The models are described in detail in the associated publication. They all assume the planet has the mass and radius of Jupiter and is on a 10-day orbit around a Solar twin. Each model has a different combination of assumed rotation rate and obliquity (aka axial tilt). The rotation rates are synchronous and 12, 4, 2, and 1 times slower than Jupiter. (Synchronous is close to 24 times slower than Jupiter.) The obliquities are 0, 10, 30, 60, and 90 degrees. Each model has two different forms for the outgoing flux maps: one that is a cylindrical projection (in the frame rotating with the planet), showing how the flux map changes throughout the planet's orbit, and one that is an orthogonal projection, showing how the dayside of the planet appears throughout the planet's orbit (as if viewed from the star). In most models a black star indicates the location of the substellar point. In the cylindrical projections from the model rotating at Jupiter's speed there is a black line indicating the substellar latitude, as the forcing pattern assumes a diurnal average and irradiates all longitudes equally.</p>
Jupiter's ground-based observations on 2018 May 24th-27th from the Very Large Telescope Imager and Spectrometer instrument
<p>The Very Large Telescope Imager and Spectrometer (VISIR) instrument on ESO's Very Large Telescope (VLT) has been used to support the NASA's Juno mission since 2016. The present dataset was collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 0101.C-0073(A)). The 2018 May 24th-27th dataset provides a comprehensive view of Jupiter's pole-to-pole thermal, chemical, and aerosol structure ; including the Great Red Spot; and the auroral-related heating in the southern polar stratosphere; after retrieval calculations.</p> <p>Here, we provide the destriped, cleaned, calibrated and projected data of 2018 May 24h to 27th dataset.</p> <p> </p> <p>For the 7.9µm filter, we have added the radial Doppler velocities files.</p>
Jupiter column base
Jupiter column base, in sandstone, bearing the figures of four gods: Jupiter, Minerva, Hercules, Ceres (?). Saint-Mard (from Luxembourg), 1st century CE. Musée du Cinquantenaire (Brussels, Belgium). Made with ReMake and ReCap Pro from AutoDesk. For more updates, please consider to follow me on Twitter at @GeoffreyMarchal. Source: Objaverse 1.0 / Sketchfab
JUPITER Study: Transapical Aortic Valve Implantation for Aortic Regurgitation
ClinicalTrials.gov study NCT01598844. IPD Sharing: Not stated. Countries: 4. Publications: 4.
The Impact of MeMed BV® on Management of Patients With Suspected Lower Respiratory Tract Infections (LRTI) in the Emergency Department (ED) and Urgent Care Center (UCC) ("JUPITER" TRIAL)
ClinicalTrials.gov study NCT05762302. IPD Sharing: NO. Countries: 2. Publications: 25.
Supplementary Information Table for J. Geophys. Res. article: A Survey of Small-Scale Waves and Wave-Like Phenomena in Jupiter's Atmosphere Detected by JunoCam
<p>Text version of the Table in the Supplementary Information file associated with the J. Geophys. Res. article by Orton et al. (2020) A Survey of Small-Scale Waves and Wave-Like Phenomena in Jupiter’s Atmosphere Detected by JunoCam. The columns provide values for various sizes and orientations associated with waves detected by the Juno spacecraft's JunoCam visible imaging instrument. The values include the perijove, PJ (orbit close approach), image number, number of wave crests detected, the mean longitude and latitude, the length and width of the wave packet, the wavelength (mean distance between wave crests), and the tilt (angle of the wave crest with respect to the direction of the wave).</p>
Juno Waves Detection of Dust Impacts near Jupiter
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics. DOI 10.1029/2019JE006367</p> <p>Abstract:</p> <p>The Juno spacecraft entered orbit at Jupiter on July 5, 2016. Since then, Juno has orbited Jupiter in high inclination orbits, crossing the ring plane near perijove 21 times. During 20 of the 21 crossings, the Waves instrument detected signals induced by dust impacts. The impact rate profiles show peaks of order 6/s around the ring plane with half width at half max ~2000-3000 km. The polarity ratio of the impact signals didn't follow the areas of the antennas exposed to dust impacts that change due to the rotation of the spacecraft, suggesting Waves detects impacts on the Juno spacecraft and not just on the Waves antennas. The impact rate profile changed during Perijove 19, when the spacecraft rotation axis was tilted to the south, increasing the area of the solar panels exposed to impacts, indicating that the detected impacts were on the spacecraft body. Grain sizes of order 1 micrometer are estimated, and the differential size distribution has a slope of -5.1.</p> <p>Notes on zip archive:</p> <p>There are subdirectories for each figure including a PDF of the figure and one or more text files with the data supporting the figure. Where the labeling in the text file is not quite complete, we've added a Fign-readme.txt file.</p> <p>Figures 9 and 10 are in the same directory as the two figures just have more of the same and all the data for both figures is in the same file.</p>
Storms and the Depletion of Ammonia in Jupiter: I. Microphysics of Mushballs
<p>This is the supporting data for the article of the same name in JGR Planets</p> <p>Microwave observations by the Juno spacecraft have shown that, contrary to expectations, the concentration of ammonia is still variable down to pressures of tens of bars in Jupiter. We show that during strong storms able to loft water ice into a region located at pressures between 1.1 and 1.5 bar and temperatures between 173K and 188K, ammonia vapor can dissolve into water ice to form a low-temperature liquid phase containing about 1/3 ammonia and 2/3 water. We estimate that, following the process creating hailstorms on Earth, this liquid phase enhances the growth of hail-like particles that we call ‘mushballs’. We develop a simple model to estimate the growth of these mushballs, their fall into Jupiter's deep atmosphere and their evaporation. We show that they evaporate deeper than the expected water cloud base level, between 5 and 27 bar depending on the assumed abundance of water ice lofted by thunderstorms and on the assumed ventilation coefficient governing heat transport between the atmosphere and the mushball. Because the ammonia is located mostly in the core of the mushballs, it tends to be delivered deeper than water, increasing the efficiency of the process. Further sinking of the condensates is expected due to cold temperature and ammonia- and water-rich downdrafts formed by the evaporation of mushballs. This process can thus potentially account for the measurements of ammonia depletion in Jupiter's deep atmosphere.</p> <p>Notes on zip archive:</p> <p>The subdirectories correspond to the figures in the article. </p>
High-Spatiotemporal Resolution Observations of Jupiter Lightning-Induced Radio Pulses Associated With Sferics and Thunderstorms
<p><strong>Abstract:</strong><br> Jupiter lightning discharges produce various kinds of phenomena including radio wave pulses at different frequencies. On 6 April 2019, the Juno Waves instrument captured an extraordinary series of radio pulses at frequencies below 150 kHz on timescales of submilliseconds. Quasi-simultaneous multi-instrument data show that the locations of their magnetic footprints are very close to the locations of UHF sferics recorded by the Juno MWR instrument. Hubble Space Telescope images show that the signature of active convection includes cloud-free clearings, in addition to the convective towers and deep water clouds that were also recognized in previous spacecraft observations of lightning source regions. Furthermore, the detections of 17 VLF/LF radio pulses suggest a minimum duration of lightning processes on the order of submilliseconds. These observations provide new constraints on the physical properties of Jupiter lightning.</p> <p><strong>Note:</strong><br> This paper was published in Geophysical Research Letters (<a href="https://doi.org/10.1029/2020GL088397">https://doi.org/10.1029/2020GL088397</a>). This page provides the digital data for all figures in this paper; please read a readme file in each figure sub-directory.</p>
Supporting data to "Tidally-induced magmatic pulses on the oceanic floor of Jupiter's moon Europa"
<p>Data used for producing figures in manuscript "Tidally-induced magmatic pulses on the oceanic floor of Jupiter's moon Europa"</p>
Video Recordings from a Stellar Occultation by Jupiter's Trojan Diomedes on November 1st, 2020
<p>Raw video recordings and their respective observer reports for the three light curves/chords.</p>
TOI-2458 b: A mini-Neptune consistent with in situ hot Jupiter formation (Additional material)
<p>Relative HARPS radial velocities and activity indicators of TOI-2458.</p>
The Emission Spectrum of the Hot Jupiter WASP-79b from HST/WFC3
<p>Supplementary material for '<strong><em>The Emission Spectrum of the Hot Jupiter WASP-79b from HST/WFC3</em></strong>'.</p> <p>This repository contains posterior probability distributions for the two cases that were investigated using the 'white' light data of WASP-79b captured by the Hubble Space Telescope using the Wide Field Camera 3. It also contains the posterior probability distributions for three spectroscopic channels. </p> <p>The two 'white' light corner plots consider two scenarios: a fixed mid-eclipse time based on the expected occurrence time and a mid-eclipse time set as a free parameter. The three spectroscopic corner plots then look at the observations divided into three equal wavelength bins of width 0.20 μm centered at 1.18, 1.38, and 1.58 μm. The spectroscopic analysis was done under the scenario of a free mid-eclipse time.</p> <p> </p>
Jupiter magnetosphere simulation data - average
<p>MHD simulation data of Jupiter's magnetosphere</p>
SolSysELTs2022 Part II: Jupiter and Saturn observations in the visible and IR with ETLs
<p>Invited talk: presentation and video recording</p>
How Bi-Modal are Jupiter's Main Aurora Zones?
<p>Provided here are ASCII dumps of the processed data that appears in the figure of the subject paper, which is under review for publication by the American Geophysical Union’s Journal of Geophysical Research, Space Physics. The PDF of the paper provided here serves to document the figures in question. </p> <p> </p> <p><strong>How Bi-Modal are Jupiter’s Main Aurora Zones?</strong></p> <p> </p> <p><strong>B. H. Mauk, J. R. Szalay, F. Allegrini, F. Bagenal, S. J. Bolton, G. Clark, J. E. P. Connerney, G. R. Gladstone, D. K. Haggerty, P. Kollmann, W. S. Kurth, C. P. Paranicas, </strong><strong>A. H. Sulaiman</strong></p> <p><strong>Key Points:</strong></p> <ul> <li>Zone I downward electron broadband acceleration sometimes has upward electrostatic potentials fully disappearing and other times enduring.</li> <li>Zone I potentials of 30-360 kV often disappear to < 10 kV with strong broadband electrons having characteristic energies of 100-400 keV.</li> <li>Why one process (electrostatic or broadband) is favored over the other at any one time remains unknown.</li> </ul> <p>Abstract</p> <p>Using Juno-measured >30 keV electrons, three regions with substantial UV emissions were identified previously for Jupiter’s main aurora (excluding the polar cap): low-latitude diffuse aurora, mid-latitude Zone I of downward acceleration, and higher latitude Zone II of bi-directional acceleration. Zone I, associated with upward magnetic field-aligned currents, was represented as bimodal: sometimes supporting coherent downward electron electrostatic acceleration and sometimes downward electron broadband acceleration, with broadband acceleration usually delivering the most intense electron energy flux at Juno. Recent observations of up-going ion beams within Zone I represent a challenge as to whether coherent electrostatic acceleration invariably accompanies broadband acceleration. Is this region strictly bi-modal, or is there a continuum between these two modes? We address these questions by combining multiple ion and electron data sources to diagnose electrostatic potentials both above and below the spacecraft. We find: 1) During Zone I downward electron broadband events, there are examples where evidence of downward electron electrostatic acceleration completely disappears and examples where it endures at some level. 2) Most often, evidence of downward electron electrostatic acceleration is strongly suppressed with strong downward electron broadband acceleration. Residual potentials most often (not always) have values small (<10 kV) compared to the electron characteristic energies of 100-400 keV. 3) Care must be exercised in these studies because plasmasheet electron precipitation spectra can mimic broadband acceleration spectra. At least for weaker auroral broadband accelerations, there is likely to be a continuum of electrostatic and broadband participation. Why either process is favored any one time is unknown.</p> <p> </p>
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Allen Brain Atlas
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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.