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430 results for “Jupiter”
Torso of an Emperor in the Guise of Jupiter
Statue from the North Carolina Museum of Art (NCMA) The placard states: 'Torso of an Emperor in the Guise of Jupiter, Roman, 1st century, Marble, Gift of Mr. and Mr.s Gordon Hanes, 1987 (86.4) [Catalogue, Torso of an Emperor in the Guise of Jupiter](https://ncartmuseum.org/art/detail/torso_of_an_emperor_in_the_guise_of_jupiter) Source: Objaverse 1.0 / Sketchfab
Jupiter
Statuette de Jupiter en bronze datée entre le 1er siècle avant n. è. et le 1er siècle découverte à Bouillac dans le Tarn-et-Garonne. Acquise en 2014 par la Ville de Toulouse avec la participation de l'association des Amis du musée Saint-Raymond, elle est conservée au musée Saint-Raymond, musée d'Archéologie de Toulouse. H. 16,8 cm l. 5,5 cm Poids 700 gr Inv. 2014.1.1 http://zone47.com/crotos/palladia/?q=28108996 Numérisation 3D par scanner 3D Artec EVA et/ou Spider par IMA Solutions SARL Source: Objaverse 1.0 / Sketchfab
Model outputs for "Modeling the day-night temperature variations of ultra-hot Jupiters: confronting non-grey general circulation models and observations"
<p>SPARC/MITgcm general circulation model outputs, including temperature structure, atomic hydrogen mixing ratio, winds, and time-resolved spectra produced by PICASO, for the paper "<strong>Modeling the day-night temperature variations of ultra-hot Jupiters: confronting non-grey general circulation models and observations" </strong>by Tan et al. (2023). </p><p>Plotting scripts in Matlab for almost all figures in the paper are provided. These scripts can be modified to read out and plot any outputs that are not shown in the paper. </p>
Dynamically coupled kinetic chemistry in brown dwarf atmospheres - II. Cloud and chemistry connections in directly imaged sub-Jupiter exoplanets
<p>Gifs of GCM output from the paper, model is Teff = 1000 K, log g = 3, M/H = 1. </p><p>The atmos_daily_2980.nc file contains the GCM NETCDF output at 2080 days.</p>
Jupiter & satellites
La planète Jupiter et 4 de ses satellites principaux les plus proches : Io, Europa, Ganymède et Callisto. ____________________ [Anaglypes](https://example3972.files.wordpress.com/2018/04/satellites-ste.jpg)[](https://example3972.files.wordpress.com/2018/03/jupiter_stereo9.jpg) Source: Objaverse 1.0 / Sketchfab
Light Curves from a Tri-chord Stellar Occultation by Jupiter's Trojan Diomedes in 2020
<p>Light curves for the three occultation chords. </p> <p> </p> <p>bender_lc.dat : occultation light curve dataset from the data provided by observer K. Bender.</p> <p>kitting_lc.dat : occultation ligth curve dataset from the data provided by observer C. Kitting.</p> <p>oesper_lc.dat : occultation light curve dataset from the data provided by observer D. Oesper. </p> <p>README.txt : column label of all light curves dataset. </p> <p> </p>
Supplementary material for Petricca et al. (2024), "Partial Differentiation of Europa and Implications for the Origin of Materials in the Jupiter System", Nature Astronomy
<p>This dataset contains the supplementary material data files associated with the <em>Nature Astronomy </em>article "Partial Differentiation of Europa and Implications for the Origin of Materials in the Jupiter System". Each folder contains the interior models associated to every case presented in the paper. The interior properties are listed in text files and can be used to reproduce most of the figures in the main text and supplementary information. The hot and cold labels refer to the different reference temperature profiles.</p>
Dataset of Effect of meteoric ions on ionospheric conductance at Jupiter
<p>This dataset contains the input parameters and the simulated results used for figures in the paper "Effects of meteoric ions on ionospheric conductance of Jupiter" by Y. Nakamura, K. Terada, C. Tao, N. Terada, Y. Kasaba, F. Leblanc, H. Kita, A. Nakamizo, A. Yoshikawa, S. Ohtani, F. Tsuchiya, M. Kagitani, T. Sakanoi, G. Murakami, K. Yoshioka, T. Kimura, A. Yamazaki and I. Yoshikawa. Detailed informations about the data files can be found in "README.txt".</p>
Exploring Jupiter's Polar Deformation Lengths with High Resolution Shallow Water Modeling
<p>Movies for simulations of non-dimensional eddy potential vorticity generated using the Pencil Code for the article "Exploring Jupiter's Polar Deformation Lengths with High Resolution Shallow Water Modeling". These movies show the Jovian North polar region in the co-rotating frame using the shallow water approximation with the gamma-plane approximation. Simulations named with a preceding A correspond to Case A (Figure 2 in the article), while those with B correspond to Case B (Figure 5 in the article). Red indicates cyclonic behavior and blue indicates anticyclonic behavior.</p> <p>Long term trends are clear for most cases as early as day 10,000. However, the dynamical behavior of the system continues to evolve well past energy equilibration. For more details regarding these simulations, please read the parent article in the Planetary Science Journal.</p>
Data for Magnetosphere-Ionosphere-Thermosphere Coupling Study at Jupiter Based on Juno's First 30 Orbits and Modeling Tools
<p>Data used in the code associated to the manuscript "Magnetosphere-Ionosphere-Thermosphere Coupling Study at Jupiter Based on Juno’s First 30 Orbits and Modeling Tools", by Al Saati et al. (2022, Journal of Geophysical Research - Space Physics, https://doi.org/10.1029/2022JA030586). Please read the documentation associated with the corresponding code.</p>
Reproduction package for Spectroscopically resolved partial phase curve of the rapid heating and cooling of the highly-eccentric Hot Jupiter HAT-P-2b with WFC3
<p>This is a basic reproduction package for the paper "<span>Spectroscopically resolved partial phase curve of the rapid heating and cooling of the highly-eccentric Hot Jupiter </span><span>HAT-P-2b with WFC3</span>"</p> <p>by [Jacobs, B.; Désert, J. -M.; Lewis, N. et al. (2024)]</p> <p>Abstract:</p> <p><span>The extreme environments of transiting close-in exoplanets in highly-eccentric orbits serve as ideal labo</span><span>ratories for testing exo-atmospheric physics. Spectroscopically resolved phase curves not only allow for the </span><span>characterization of their thermal response to irradiation changes but also unveil phase-dependent atmospheric </span><span>chemistry and dynamics.</span></p> <p><span>We observed a partial phase curve of the highly-eccentric close-in giant planet HAT-P-2b (</span><span>e</span> <span>=</span> <span>0</span><span>.</span><span>51023)</span><br><span>with the Wide Field Camera 3 (WFC3) aboard the</span> <span>Hubble Space Telescope</span><span>.</span> <span>Using these data, we update </span><span>the planet’s orbital parameters and radius, and we retrieve high-frequency pulsations consistent with those re</span><span>ported in Spitzer data. We find that the peak in planetary flux occurs at 6</span><span>.</span><span>7</span> <span>±</span> <span>0</span><span>.</span><span>6 hr after periastron, with a </span><span>heating timescale of 9</span><span>.</span><span>0</span><span>+</span><span>3</span><span>.</span><span>5</span><br><span>−</span><span>2</span><span>.</span><span>1</span> <span>hr, and a cooling timescale of 3</span><span>.</span><span>6</span><span>+</span><span>0</span><span>.</span><span>7</span><span>−</span><span>0</span><span>.</span><span>6</span> <span>hr. We compare the light-curve to a suite of</span><br><span>1-dimensional and 3-dimensional forward models, varying the planet’s chemical composition. The strong con</span><span>trast in flux increase and decrease timescales before and after periapse indicates an opacity term that emerges </span><span>during the planet’s heating phase. We suggest that more emerging H</span><span>−</span> <span>than expected from chemical equilibrium </span><span>models could be the reason for the mismatch between models and the data.</span></p> <p><span>We used a common-mode based method that does not assume a functional form to extract phase-resolved </span><span>spectra. The analysis of these spectra is challenging because of the unknown accuracy of the spectral slope and </span><span>absolute flux levels. The phase-resolved spectra are largely featureless, possibly indicating an inhomogeneous </span><span>dayside.</span> <span>However, we identified an anomalously high flux in the spectroscopic bin that coincides with the </span><span>hydrogen Paschen</span> <span>β</span> <span>line and that is potentially connected to the planet’s orbit.</span> <span>We exclude an instrumental </span><span>origin and we discuss several alternative, astrophysical origins.</span></p>
Repository for Jupiter Equatorial Zone Disturbance Data
<p>Antuñano et al. (2018) used Jupiter infrared data captured by 8 different ground-based instruments mounted on the Infrared Telescope Facility (IRTF) on Maunakea and Very Large Telescope (VLT) in Paranal between 1984 and 2017, to investigate a pattern of cloud clearance events at Jupiter's equatorial zone at 5 µm.This repository contains (i) cylindrical maps of Jupiter's 5-µm images from 1999-2000 and 2006-2007 captured by NSFCam and NSFCam2 instruments, respectively, mounted on the IRTF, showing Jupiter's Equatorial Zone disturbance, and (ii) a data file showing the brightness scans from ±7° latitude as a function of time used to build Figure 2.</p> <p>DATA</p> <p>As descibed in Antuñano et al. (2018), the normalised average brightness from 1984-2017 was used to charcterise three different cloud clearance events of Jupiter's equatorial zone at 5 µm. The normalised average brightness of the equatorial zone between ±7° latitude is given in "Brightness_scans_1984-2017.dat", where the first column represents the Julian date, the second column represents the latitude in planetocentric degrees, the third column represents the normalised average brightness and the fourth column gives the standard deviation of the normalised average brightness.</p>
Structure and Evolution of Internally Heated Hot Jupiters
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017ApJ...844...94K/abstract">Komacek & Youdin (2017)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-4357/aa7b75">10.3847/1538-4357/aa7b75</a></p>
Implementation of Aerosol Mie Scattering in POSEIDON with Application to the hot Jupiter HD 189733 b's Transmission, Emission, and Reflected Light Spectrum - Supplementary Material
<p>Supplementary material to 'Implementation of Aerosol Mie Scattering in POSEIDON with Application to the hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum'</p> <p>This zenodo repository corresponds to the updates to POSEIDON presented in Mullens et al 2024, as well as the benchmark retrievals preformed on archival HD 189733 b. </p> <p>In the upper level of the repository we have data products mentioned in the paper:</p> <p>aersosol_database.pdf <br>Aerosol-Database-Readme.txt<br>aerosol_database.hdf5</p> <p>There are then three directories (here as zip files): </p> <p>Aerosol-Datbase<br>- This folder contains the aerosol properties for aerosols in Table 1 in the paper. It contains the aerosol-database.hdf5 which contains the precomputed aerosol properties that POSEIDON utilizes in forward models and retrievals, a folder containing the npy files that have individual precomputed aerosol properties (used to generate the hdf5 file), a pdf containing the refractive indices + precomputed aerosol properties for each aerosol in the database (png versions of these figures are available in the Aerosol-Optical-Properties-Pngs folder), the refractive index txt files for each aerosol, and a readme file that contains information on each aerosol in the database (such as aerosol name, polymorph, crystalline or amorphous, crystal shape, information on samples used in refractive index references, and exoplanet/planetary science specific references). </p> <p>HD-189733b-Retrievals<br>- Contains retrieval scripts and retrieval results for the transmission, emission, and emission+reflection retrievals in the paper. Also has the notebooks used to make the figures in the paper.</p> <p>POSEIDO-V1-2<br>- Contains the POSEIDON module used to run retrievals and generate figures, and corresponds to POSEIDON version 1.2. Also contains a folder containing tutorial notebooks for new features introduced into POSEIDON version 1.2. Included in this repository for posterity.</p>
Code for 'Revealing the Local Time Structure of the Alfven Radius and travel times in Jupiter's magnetosphere'
Open the record for dataset details and reuse information.
Confirmation of four hot Jupiters detected by TESS using follow-up spectroscopy from MaHPS at Wendelstein together with NEID and TRES
<p>Supplementary material to the paper 'Confirmation of four hot Jupiters detected by TESS using follow-up spectroscopy from MaHPS at Wendelstein together with NEID and TRES':</p> <p>Fig. Z1 - Z4: Fit of the photometric lightcurves (Sec. 2.2)</p> <p>ZT1 -ZT4: Tables showing the parameters, the prior distribution and the posteriors for the four targets after performing a joint fit with the Python package 'juliet' (Sec. 5.1)</p> <p>Fig. Z5_6: S/N values for the observations taken with MaHPS (Sec. 3.2.1)</p> <p>Fig. Z7: O-C diagrams for the search of TTVs (Sec. 5.3.2)</p> <p> </p> <p> </p>
Jupiter's Rotation, by Vishal Sharma, India
<p>Third place in the 2021 IAU OAE Astrophotography Contest, category Galilean moons: Jupiter’s Rotation, by Vishal Sharma, India.</p> <p>This time-lapse beautifully shows the rotation of Jupiter and the passage of two Galilean moons on the right side of the frame. Jupiter completes one rotation in just under 10 hours and we see as the Great Red Spot makes its way from left to right. The two moons travel a noticeable fraction of their orbit in this short time. This image was taken in 2020 in the North of India.</p> <p>Credit: Vishal Sharma/IAU OAE</p>
Jupiter Moon's Movie2, by Nicolas Hurez, Paul-Antoine Matrangolo, and Carl Pennypacker, United States of America
<p>Second place in the 2021 IAU OAE Astrophotography Contest, category Galilean moons.</p> <p>This sequence shows the orbit of the four Galilean moons around the planet Jupiter. Almost two entire orbits of the innermost moon, Io, can be seen, with the other moons (Europa and Ganymede, but in particular Callisto) being further away, orbiting noticeably slower. The images were obtained in 2018 with the Las Cumbres Global Observatory at different locations on Earth, allowing a continuous sequence of images over approximately half a week without gaps during the day. With clear skies and over the course of several nights, the motion of the Galilean moons can also be observed with binoculars (ideally steady your elbows on a surface).</p> <p>Credit: Nicolas Hurez, Paul-Antoine Matrangolo and Carl Pennypacker/IAU OAE</p>
Jupiter, Io and its shadow, by Ralf Burkart, Germany
<p>First place in the 2021 IAU OAE Astrophotography Contest, category Galilean moons.</p> <p>This time-lapse of Jupiter taken in 2017 from Germany beautifully illustrates the transit of one of the Galilean moons, Io, in front of Jupiter. As this is simply a moon casting a shadow on a planet it is equivalent to a lunar eclipse on Earth observed from further away. While the shadow of the moon is clearly visible from the beginning, it might be difficult to spot the moon itself against the background of the beautiful atmospheric bands of Jupiter the first time the video is seen. Watching it repeatedly allows appreciating the rapid motion and rotation in this fantastic observation.</p> <p>Credit: Ralf Burkart/IAU OAE</p>
Triple shadow phenomena on Jupiter, Saturn and Uranus from 1000 CE to 3000 CE
<p>I computed all triple shadow phenomena of the major moons with their planet from 1000 CE to 3000 CE. I found 315 of such phenomena occurring on Jupiter, 303 on Saturn and 151 on Uranus. During the 2001 year period Saturn experiences 1 quadruple shadow phenomena meanwhile Uranus experiences 3 of such. I computed all shadow events of the Galilean moons with Jupiter, their mutual eclipses and the planet’s elongation from 1000 CE to 3000 CE with Occult 4.10.1.0 (files updated: 2020 March 20). I repeated the same procedure for Tethys, Dione, Rhea, Titan and Iapetus with Saturn and Miranda, Ariel, Umbriel, Titania and Oberon with Uranus. I then filtered the results to find triple and quadruple shadow events within the satellites and their respective primaries. Finally, I added the planet’s elongation for the event’s date above found and mutual eclipses only occurring during a triple or quadruple shadow event on the planet. I assumed that the Gregorian calendar commenced in 1582 October 4. Before that date, I used the Julian calendar. All times are in Universal Time. Minutes are rounded to the nearest tenth of a minute. For convenience, I used Arabic numbers to designate all satellites instead of Roman ones.</p>
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OpenNeuro
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