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430 results for “Jupiter”
Giant Tidal Tails of Helium Escaping the Hot Jupiter HAT-P-32 b
<p>This dataset contains materials presented in the paper ``Giant Tidal Tails of Helium Escaping the Hot Jupiter HAT-P-32 b'' (Zhang et al. 2023) accepted for publication by Science Advances. Please cite this paper and the Zenodo repository if these data are used in your work.</p> <p>Description of these files: </p> <ul> <li><strong>HPF_data.zip</strong> includes all 77 observed HPF spectral data of HAT-P-32 A+b.</li> <li><strong>HAT-P-32b_properties.csv</strong> includes our measured spectroscopic and physical properties of the planetary system. Columns of this file are explained in a README file <strong>README_HAT-P-32b_properties.dat</strong></li> <li><strong>3d_simulation_EW_vs_orbital_phase.dat</strong> includes the helium excess equivalent widths as a function of the planet's orbital phase, as predicted by our 3D hydrodynamic simulations</li> <li><strong>3d_simulation_orbital_phase_vs_helium_central_wavelength.dat</strong> includes the central wavelength of helium excess spectral feature (in the stellar restframe) as a function of the planet's orbital phase, as predicted by our 3D hydrodynamic simulations. </li> </ul>
Spectra and retrieval data from CO and HCN observations of Jupiter with ALMA (project 2016.1.01235.S)
<p>Spectra and retrieval data from:</p> <p>Title: Evidence for auroral influence on Jupiter's nitrogen and oxygen chemistry revealed by ALMA<br> Authors: T. Cavalié, L. Rezac, R. Moreno, E. Lellouch, T. Fouchet, B. Benmahi, T. K. Greathouse,<br> J. A. Sinclair, V. Hue, P. Hartogh, M. Dobrijevic, N. Carrasco, Z. Perrin<br> Journal: Nature Astronomy<br> Year: 2023</p> <p>########################<br> # Description of files #<br> ########################</p> <p>CO_data/<br> latitudes_CO.dat: planetocentric latitudes of the 540 pointings from which the CO spectra have been extracted<br> spectrum_*.dat : CO spectra, one per pointing. Frequency in GHz and continuum-subtracted flux density in Jy/beam<br> profiles_*.dat : vertical profiles, one per pointing. Pressure in mbar, temperature in K (local average, see paper for details), and retrieved CO volume mixing ratio</p> <p>HCN_data/<br> latitudes_HCN.dat: planetocentric latitudes of the 557 pointings from which the HCN spectra have been extracted<br> spectrum_*.dat : HCN spectra, one per pointing. Frequency in GHz and continuum-subtracted flux density in Jy/beam<br> profiles_*.dat : vertical profiles, one per pointing. Pressure in mbar, temperature in K (local average, see paper for details), and retrieved HCN volume mixing ratio</p> <p> </p>
Products and Models for "A broadband thermal emission spectrum of the ultra-hot Jupiter WASP-18b"
<p>Close-in giant exoplanets with temperatures greater than 2,000 K (“ultra-hot Jupiters”) have been the subject of extensive efforts to determine their atmospheric properties using thermal emission measurements from the Hubble and Spitzer Space Telescopes1–3. However, previous studies have yielded inconsistent results because the small sizes of the spectral features and the limited information content of the data resulted in high sensitivity to the varying assumptions made in the treatment of instrument systematics and the atmospheric retrieval analysis3–12. Here we present a dayside thermal emission spectrum of the ultra-hot Jupiter WASP-18b obtained with the NIRISS13 instrument on JWST. The data span 0.85 to 2.85 μm in wavelength at an average resolving power of 400 and exhibit minimal systematics. The spectrum shows three water emission features (at <6σ confidence) and evidence for optical opacity, possibly due to H-, TiO, and VO (combined significance of 3.8σ). Models that fit the data require a thermal inversion, molecular dissociation as predicted by chemical equilibrium, a solar heavy-element abundance (“metallicity”, M/H = 1.03-0.51+1.11 x solar), and a carbon-to-oxygen (C/O) ratio less than unity. The data also yield a dayside brightness temperature map, which shows a peak in temperature near the sub-stellar point that decreases steeply and symmetrically with longitude toward the terminators.</p>
Altar to Jupiter and other gods
Limestone altar with a long vague inscription, set in a simple frame. Above the inscription two animals are running towards the center and are depicted in a low relief. Between them stands probably a tree. National Museum of Antiquities, Leiden, the Netherlands; Reg. No. Pb 1; limestone; 119x73,5x50cm; 1165kg; Roman period; 174 AD; Vechten, the Netherlands; legacy January 1818 Source: Objaverse 1.0 / Sketchfab
Roman Jupiter Column Base
Half octagon with reliefs of the Gods of the Week, probably from a Jupiter column base. Found at Great Chesterford, England. Now located in British Museum. Photos taken November 2018 with Sony a6000 and processed in Agisoft Photoscan. https://www.britishmuseum.org/research/collection_online/collection_object_details.aspx?objectId=1363387&partId=1 Source: Objaverse 1.0 / Sketchfab
JUPITER - Crestor 20mg Versus Placebo in Prevention of Cardiovascular (CV) Events
ClinicalTrials.gov study NCT00239681. IPD Sharing: Not stated. Countries: 27. Publications: 32.
A survey of small-scale waves and wave-like phenomena in Jupiter's atmosphere detected by JunoCam
Open the record for dataset details and reuse information.
Velocity field of Jupiter's Great Red Spot in December 2016
Open the record for dataset details and reuse information.
Dataset for Angular Dependence and Spatial Distribution of Jupiter's Centimeter-Wave Thermal Emission from Juno's Microwave Radiometer
<p>This dataset comprises all processed data (in HDF5 format) used in figures and discussion in the paper "Angular Dependence and Spatial Distribution of Jupiter's Centimeter-Wave Thermal Emission from Juno's Microwave Radiometer".</p>
Dataset for "Ray Tracing of Whistler Mode Waves in Jupiter's Magnetosphere"
<p>Dataset for "Ray Tracing of Whistler Mode Waves in Jupiter's Magnetosphere". Containing all the ray tracing results that are used in this paper. </p>
Simulation data for "A new convective parameterization applied to Jupiter: implications for water abundance near the 24deg N region"
<p>Simulation outputs and initialization for the journal article titled "A new convective parameterization applied to Jupiter: implications for water abundance near the 24º N region" by Sankar & Palotai.</p>
Repository for the paper "Stability of the Jupiter southern polar vortices inspected through vorticity using Juno/JIRAM data"
<p>This repository contains all the *img and *lbl files that have been used in the analysis reported in "Stability of the Jupiter southern polar vortices inspected through vorticity using Juno/JIRAM data". Please see the text for details. </p>
The oscillatory motion of Jupiter's polar cyclones results from vorticity dynamics - Movies S1, S2
<p>Movie S1: An animation of the observed trajectories of the south polar cyclones, as illustrated in Fig. 2a, along the 45-months of observations. The blue arrows represent the estimated net forces on the cyclones, as presented in Fig. 4.</p> <p>Movie S2: An animation of the simulated trajectories of the south polar cyclones, as illustrated in Fig. 5a, along 45-months.<br> The blue arrows represent the net forces on the cyclones.</p>
Basic fragment of Jupiter's column
Basic fragment of Jupiter's column, in limestone, with representation of Venus in the center, Juno and his peacock on the right, statue of Apollo archer running and a dog sitting. Fontaine-Valmont (from Hainaut). Musée d'Art et d'Histoire (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
Size evolution of Jupiter's Great Red Spot
<p>This dataset contains the historical size measurements (length and width) of Jupiter's Permanent Spot (PS) and the Great Red Spot (GRS) and its Hollow. It also contains the fits to the GRS shrinkage rates for different epochs. The second dataset gives PS and GRS zonal velocities in meters per second).</p>
Long-term SW simulations of Jupiter's GRS
<p>Data and input files for the SW2 software regarding the simulations presented in "The origin of Jupiter’s Great Red Spot".</p>
Products for "Hydrogen sulfide and metal-enriched atmosphere for a Jupiter-mass exoplanet"
<p>Data and model for JWST transit observation of HD 189733b using NIRCam (GO 1633, PI: Drake Deming) from paper "Hydrogen sulfide and metal-enriched<br>atmosphere for a Jupiter-mass exoplanet" (Fu et al. 2024).</p>
Supporting material to "Effect of magnetospheric conditions on the morphology of Jupiter's UV main auroral emission, as observed by Juno-UVS"
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Nightside Contamination of Hot Jupiter Transmission Retrievals - Supplementary Material
<p>Supplementary material for '<em>From the Shadows: The Impact of Nightside Thermal Emission on Ultra-hot Jupiter Transmission Spectra Retrievals</em>' - ApJ (2024).</p> <p>This repository contains the full posterior probability distributions from the retrieval simulations in Kappelmeier, MacDonald, & Lewis (2024). The file names for the 12 corner plots correspond to the model assumptions and data used as follows:</p> <ul> <li><strong>TransOnly</strong> / <strong>TransPlusNightside</strong>: The former transmission models neglect nightside thermal emission (i.e. these correspond to 'biased' retrievals) while the latter include nightside emission.</li> <li><strong>N_trans_X</strong>: 'X' corresponds to the number of transits per instrument mode. This is either 1, 2, or 3 transits per mode.</li> <li><strong>NIRISS_SOSS / NIRSpec_G395H / MIRI_LRS / All_Instruments</strong>: The simulated JWST dataset used for the retrieval. The specific names are for single-instrument retrievals, while 'All_Instruments' corresponds to the combination of NIRISS SOSS, NIRSpec G395H, and MIRI LRS.</li> </ul> <p>Each corner plot shows the correlations between pairs of retrieved parameters and marginalized histograms for each parameter. The green lines are the true parameter values used to generate the simulated JWST datasets. The solid blue lines are the median retrieved value for each parameter, while the blue dashed lines are the ±1σ confidence intervals. The shaded purple contours in the correlation plots are, from darkest to lightest, the 1σ, 2σ, and 3σ confidence levels.</p> <p>For any questions, please contact: jak485@cornell.edu</p>
The ouput simulation data of the Exo-FMS GCM and of the post-processing with gCMCRT for Effects of the internal temperature on vertical mixing and on cloud structures in Ultra Hot Jupiters
<p>The datasets contains the ouput simulation data of the Exo-FMS GCM and of the post-processing with gCMCRT for Effects of the internal temperature on vertical mixing and on cloud structures in Ultra Hot Jupiters</p> <p>Context. The vertical mixing in hot Jupiter atmospheres plays a critical role in the formation and spacial distribution of cloud particles<br>in their atmospheres. This affects the observed spectra of a planet through cloud opacity, which can be influenced by the degree of<br>cold trapping of refractory species in the deep atmosphere.<br>Aims. We aim to isolate the effects of the internal temperature on the mixing efficiency in the atmospheres of Ultra Hot Jupiters (UHJ)<br>and the spacial distribution of cloud particles across the globe.<br>Methods. We couple a simplified tracer based cloud model, picket fence radiative-transfer scheme and mixing length theory to the<br>Exo-FMS general circulation model. We run the model for five different internal temperatures at typical UHJ atmosphere system<br>parameters.<br>Results. Our results show the convective eddy diffusion coefficient remains low throughout the vast majority of the atmosphere, with<br>mixing dominated by advective flows. However, some regions can show convective mixing in the upper atmosphere for colder interior<br>temperatures. The vertical extent of the clouds is reduced as the internal temperature is increased. Additionally, a global cloud layer<br>gets formed below the radiative-convective boundary (RCB) in the cooler cases.<br>Conclusions. Convection is generally strongly inhibited in UHJ atmospheres above the RCB due to their strong irradiation. Convective<br>mixing plays a minor role in keeping cloud particles aloft in ultra hot Jupiters with warm interiors. Our results suggest isolated upper<br>atmosphere regions above cold interiors may exhibit strong convective mixing, allowing aerosols to be better retained in these areas.</p>
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