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430 results for “Jupiter”
Upward, MeV-class electron beams over Jupiter's Main Aurora; Selected data for
<p>This submission provides selected ASCII data that is utilzed in a scientific study entitled: "Upward, MeV-class electron beams over Jupiter’s Main Aurora". A PDF of the manuscript is included here. The 13 authors of this study are identified in the PDF manuscirpt. The data files are labeled according to the figure numbers and panels used in the manuscript. The PDF of the paper serves to document the qualities of the data submitted. The abstract of the manuscript is as follows: </p> <p>Abstract: Jupiter’s poleward (Zone II) main aurora exhibits bi-directional electron acceleration; upward acceleration dominates but downward acceleration generates strong aurora. During Juno’s first perijove (PJ1), the upward acceleration manifested as narrow electron angular beams (within ~5 of the magnetic field) over the 30-1200 keV energy range of Juno’s Jupiter Energetic Particle Detector Investigation (JEDI). These beams can be simply connected (non-uniquely) to >10 to perhaps 100’s of MeV electrons that penetrated the radiation shielding of the camera head of the Magnetometer Investigation’s Advanced Stellar Compass (ASC). The most intense of those multiple MeV populations are shown to have been highly directional and propagating upwards. How auroral processes generate such beams is unknown. With azimuthal symmetry assumed (not demonstrated here), these beams provided >1026 s-1 of >30 keV electrons to Jupiter’s vast magnetosphere, a possibly critical and dominating source of energetic electrons to that region and ultimately to Jupiter’s radiation belts.</p>
Chandra HRC-I Jupiter X-ray data set
<p>Data set to supplement code scripts contained in the repository: https://github.com/SeanMcEntee/cxo_goes_disk_study</p> <p> </p>
Spherical harmonic models of the gravity field of Jupiter
<p>This archive contains published spherical harmonic models of the gravity field of Jupiter. The coefficients are to be used with unnormalized spherical harmonic functions that exclude the Condon-Shortely phase factor of (-1)^m, and the file is formatted in a manner to be read by the <a href="https://shtools.github.io/SHTOOLS/">pyshtools</a> software (using format='shtools'). The header of the file contains the reference radius, GM, GM uncertainty, and maximum degree of the spherical harmonic expansion (all in SI units).</p> <p>* Kaspi2023.sh (value of GM provided by Y. Kaspi, personal communication)</p>
Supporting Data - Double Ridge Formation over Shallow Water Sills on Jupiter's Moon Europa
<p>This archive contains data produced in support of R. Culberg, D. M. Schroeder, G. Steinbrügge, Double Ridge Formation Over Shallow Water Sills on Jupiter’s Moon Europa, <em>Nature Communications</em>, 2022. This includes the WorldView imagery in Figure 1, the reprocessed radargrams underlying the radar analysis and inversion, and outputs of all inversion and sensitivity test runs. See the README file for a complete description of the files available in this archive.</p>
Signatures of Nitrogen Chemistry in Hot Jupiter Atmospheres - Posteriors
<p>Supplementary material for 'Signatures of Nitrogen Chemistry in Hot Jupiter Atmospheres', ApJL, 2017.</p> <p>Contains the posterior probability distributions resulting from atmospheric retrievals of WASP-31b, WASP-63b, and HD 209458b.</p>
Data for Figures in "Unexpected Long-Term Variability in Jupiter's Tropospheric Temperatures
<p>This repository provides the data submitted by the primary author that were used to create Figures 1, 2, 3, 4 and 5 in the text for the article: <strong>"Unexpected Long-Term Variability in Jupiter's Tropospheric Temperatures", by </strong> Glenn S. Orton, Arrate Antuñano, Leigh N. Fletcher, James Sinclair, Thomas Momary, Takuya Fujoyoshi, Padma Yanamandra-Fisher, Padraig T. Donnelly, Jennifer Greco, Anna Payne, Kimberly Boydstun, Laura Wakefield.</p> <p>The repository consists of five files in text (ASCII) format: (1) User Guide to Data (16 kb), (2) figure1_data.txt (1.5 MB), (3) figure2_data.txt (142 kb), figure4_data.txt (61 kb), and figure5_data.txt (59 kb). Data for Figure 3 are provided in the User Guide.</p>
Gemini/TEXES Spectroscopic Observations of Jupiter (March 12-14 2017)
<p>This dataset contains Gemini/TEXES spectroscopic maps of Jupiter, acquired between March 12-14 2017 in support of NASA's Juno mission. The data and its reduction/analysis is fully described in <em>Fletcher et al. (2020), Jupiter's Equatorial Plumes and Hot Spots: Spectral Mapping from Gemini/TEXES and Juno/MWR, Journal of Geophysical Research - Planets.</em></p> <p>As described in that paper, TEXES scan maps were acquired in seven groups (three on March 12, three on March 13, and one on March 14), with each group containing scan maps at 9 spectral settings (539, 587, 745, 819, 900, 960, 1165, 1248 and 2145 cm-1). Each setting spans approximately 10-20 cm-1, with variable spectral resolution as described in the article. </p> <p>Each scan map has been geometrically registered (i.e., latitudes, longitudes, and emission angles have been assigned), wavelength calibrated, and destriped. Radiometric calibration is in its raw form, based on TEXES observations of the telluric sky emission and a blank card in the instrument. However, we found it necessary to scale these spectra to match observations from Cassini/CIRS, using the following scale factors for all spectra:</p> <ul> <li>fac538= 0.9</li> <li>fac587= 0.687705</li> <li>fac744= 0.872656</li> <li>fac819= 0.600016</li> <li>fac901= 0.544984</li> <li>fac960= 0.427803</li> <li>fac1161=0.636066</li> <li>fac1248=1.0</li> <li>fac2145=1.0</li> </ul> <p>The format of the individual files (IDL "save" files) is as follows:</p> <ul> <li>EMMIMG FLOAT = Array[721, 361] - emission angles for each point in the map</li> <li>HDR STRING = Array[126] - header containing information about each observation</li> <li>IMAGE_REDUCT FLOAT = Array[149, 183] - summed image of Jupiter from all points in a spectral scan.</li> <li>IMG FLOAT = Array[374, 721, 361] - cylindrically mapped Jupiter data at 374 wavenumber positions.</li> <li>OLAT FLOAT = Array[361] - planetographic latitudes</li> <li>OLON FLOAT = Array[721] - System III West longitudes.</li> <li>SKY FLOAT = Array[374] - sky emission on the wavenumber grid.</li> <li>SUBLAT FLOAT - sub-observer latitude</li> <li>SUBLON FLOAT - sub-observer longitude</li> <li>TRUESKY FLOAT = Array[374] - sky emission on the wavenumber grid.</li> <li>WAVENUMBER DOUBLE = Array[374] - wavenumber array</li> </ul>
Reproduction package for "A strong H− opacity signal in the near-infrared emission spectrum of the ultra-hot Jupiter KELT-9b"
<p>This is a basic reproduction package for the paper "A strong H− opacity signal</p><p>in the near-infrared emission spectrum of the ultra-hot Jupiter KELT-9b"</p><p>by [Jacobs, B.; Désert, J. -M.; Pino, L. et al. (2022)](https://doi.org/10.1051/0004-6361/202244533).</p><p> </p><p>Abstract:</p><p>We present the analysis of a spectroscopic secondary eclipse of the hottest transiting exoplanet detected to date, KELT-9b, obtained with the Wide Field Camera 3 aboard the <i>Hubble</i> Space Telescope. We complement these data with literature information on stellar pulsations and <i>Spitzer</i>/Infrared Array Camera and Transiting Exoplanet Survey Satellite eclipse depths of this target to obtain a broadband thermal emission spectrum. Our extracted spectrum exhibits a clear turnoff at 1.4 μm. This points to H− bound-free opacities shaping the spectrum. To interpret the spectrum, we perform grid retrievals of self-consistent 1D equilibrium chemistry forward models, varying the composition and energy budget. The model with solar metallicity and C/O ratio provides a poor fit because the H− signal is stronger than expected, requiring an excess of electrons. This pushes our retrievals toward high atmospheric metallicities ([M/H] = 1.98−0.21+0.19) and a C/O ratio that is subsolar by 2.4<i>σ</i>. We question the viability of forming such a high-metallicity planet, and therefore provide other scenarios to increase the electron density in this atmosphere. We also look at an alternative model in which we quench TiO and VO. This fit results in an atmosphere with a slightly subsolar metallicity and subsolar C/O ratio ([M/H] = −0.22−0.13+0.17, log (C/O) = −0.34−0.34+0.19). However, the required TiO abundances are disputed by recent high-resolution measurements of the same planet.</p>
Jupiter, Venus, Moon Conjunction
<p>Honorable mention in the 2023 IAU OAE Astrophotography Contest, category Still images with smartphones-mobile devices: Jupiter, Venus, Moon Conjunction, by Joslynn Appel.</p> <p>Captured with a smartphone in February 2023, over the skies of Luzerne County, Pennsylvania, USA, this photograph offers a glimpse into a conjunction, an enthralling astronomical phenomenon that occurs when two or more celestial objects are seen in close proximity in the sky from our perspective, despite the objects not being physically near to each other. In this image, the brilliance of Jupiter (top), the allure of Venus (middle), and the familiar glow of our Moon (bottom) dance together against a backdrop of delicate clouds and a treeline silhouette, making it a moment worth treasuring.</p> <p>Credit: Joslynn Appel/IAU OAE (<a href="https://creativecommons.org/licenses/by/4.0/legalcode">CC BY 4.0</a>)</p> <p> </p>
Products and Models for "Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b"
<p>Hot Jupiters are among the best-studied exoplanets, but it is still poorly understood how their chemical composition and cloud properties vary with longitude. Theoretical models predict that clouds may condense on the nightside and that molecular abundances can be driven out of equilibrium by zonal winds. Here we report a phase-resolved emission spectrum of the hot Jupiter WASP-43b measured from 5-12 μm with JWST's Mid-Infrared Instrument (MIRI). The spectra reveal a large day-night temperature contrast (with average brightness temperatures of 1524±35 and 863±23 Kelvin, respectively) and evidence for water absorption at all orbital phases. Comparisons with three-dimensional atmospheric models show that both the phase curve shape and emission spectra strongly suggest the presence of nightside clouds which become optically thick to thermal emission at pressures greater than ~100 mbar. The dayside is consistent with a cloudless atmosphere above the mid-infrared photosphere. Contrary to expectations from equilibrium chemistry but consistent with disequilibrium kinetics models, methane is not detected on the nightside (2σ upper limit of 1-6 parts per million, depending on model assumptions).</p>
The Eurybates family of the Jupiter Trojan asteroids: members, orbital and spectral properties
<p>This dataset contains identified members of the Eurybates family, a collisional family of the Jupiter Trojans.</p> <p>The members were identified in Marschall et al 2022 (Implications for the collisional strength of Jupiter Trojans from the Eurybates family) using the hierarchical clustering method (HCM).</p> <p>Two tables presented in the accepted manuscript are available here in machine-readable form.</p> <p><strong>Table 3.</strong> List of all 400 Eurybates family members identified by the hierarchical clustering method (HCM) including the likely interloper (5258) Rhoeo (see discussion in Sec. 2). The table gives the asteroid number (nr.), the provisional designation (prov. des.), the absolute magnitude (H), the diameter (D), as well as the proper semi-major axis (a_prop), eccentricity (e_prop), and inclination (i_prop).</p> <p><strong>Tabel 4. </strong>Color data for Eurybates family members identified by the hierarchical clustering method (HCM) including the likely interloper (5258). The table gives the asteroid number (nr.), the provisional designation (prov. des.), the absolute magnitude (H), the diameter (D), as well as the g-i color from the Sloan Digital Sky Survey, the spectral slopes between 0.3$ to 0.9 \mu m (S), and the g-r color from the Zwicky Transient Facility Observations, ZTF.</p> <p> </p>
A Survey of Electron Conics at Jupiter Utilizing the JADE-E Data During Science Orbits 01, 03-30
<p>This dataset provides Figure 1 from the AGU <em>JGR: Space Physics</em> article of the same name as a PNG image. It also includes text files with the data to reproduce Figures 2-13 in the same AGU <em>JGR:Space Physics</em> article.</p> <p><strong>Key Points:</strong></p> <ol> <li>We surveyed the JADE-E data for science orbits 01, 03-30 and found upward, downward, and bidirectional electron conics 2.5% of the time</li> <li>We observed all electron conics to occur most often at altitudes of 0.3-0.4 R<sub>J</sub> and local times of 15-16h</li> <li>We observed all electron conic types to have energies greater than 0.7 keV below an altitude of 0.5 R<sub>J</sub> and over the main auroral region</li> </ol> <p><strong>Abstract</strong></p> <p>We present a survey of electron conics over Jupiter’s high latitude regions utilizing 22.6 hours of data from the Jovian Auroral Distribution Experiment electron (JADE-E) instrument aboard NASA’s Juno spacecraft during science orbits 01 and 03-30. We observed electron conics for about 2.5% of this time and characterized them into three types based on their direction of motion along Jupiter’s magnetic field lines: upward, downward, and bidirectional. We observed the upward electron conics most often and at energies of 0.057-80.1 keV, while we observed the downward electron conics least often and at energies of 0.073-1.2 keV. We observed bidirectional electron conics mostly around the same times and places as the upward electron conics having energies of 0.081-49.6 keV. We observed all electron conic types to occur mostly at altitudes 0.3-0.4 R<sub>J</sub> and local times 15-16h. Furthermore, we observed all electron conic types to have energies greater than 0.7 keV below an altitude of 0.5 R<sub>J</sub> and over the main auroral region.</p> <p> </p>
Jupiter Notebook and example data for "Prospects for a camera-based detector for Neutron Reflectometry"
<p>We report the outcome of a proof-of-principle (IPTS-29165) neutron reflectivity measurement obtained using a neutron scintillator and a Photonis (brand) camera. We were motivated to test this technology because it provides much better spatial resolution and count rate capability than the BL4A <sup>3</sup>He position sensitive detector (Table 1). The report describes the detector setup, challenges encountered, a reflectivity measurement and next steps.</p> <p>Two example measurements are provided and a Jupyter Notebook to create a NumPy binary file consisting of event positions and times.</p>
Extended Files for "Lessons from Hubble & Spitzer: 1D Self-Consistent Model Grids for 19 Hot Jupiter Emission Spectra"
<p>This directory includes extended files for Wiser et al. 2024, "Lessons from Hubble & Spitzer: 1D Self-Consistent Model Grids for 19 Hot Jupiter Emission Spectra." </p> <p>Files:</p> <ul> <li><strong>Extended Planet Figures:</strong> For each of the 20 planets discussed in the manuscript, <em>[PlanetName].pdf </em>includes figures showing the secondary eclipse spectra and parameter estimations for each model scenario. A file for Kepler-13Ab illustrates our grid models' inability to explain the WFC3 and Spitzer observations simultaneously. </li> <li><strong>Internal Temperature Tests:</strong><em> InternalTemperatureTests.pdf</em> includes figures illustrating our inability to constrain an atmosphere's internal temperature with these model grids and the WFC3 and Spitzer observations.</li> <li><strong>Parameter Estimates .csv Tables:</strong> <ul> <li>Both .csv files include planet and star parameters (temperatures, radii, mass, logg, semimajor axis) and parameter ranges for each planet grid. They also include parameter estimations for each model scenario. Listed are the medians of each parameter's posterior probability distribution and pos/neg values encompassing the one-sigma confidence region. This information is shown visually in the extended planet figures. </li> <li><em>fiducial_stats.csv</em> includes parameter estimations for the fiducial model scenario. For planets with multiple solutions (as described in Wiser et al. 2024), multiple rows detail each solution. There is also a "limit" flag for parameters with an upper limit, lower limit, or unconstrained (UL, LL, or UC, respectively).</li> <li><em>nonfiducial_stats.csv </em>includes parameter estimates for all other model scenarios. This table does not account for multiple solutions or "limit" flags. </li> </ul> </li> <li>For complete model grids, please contact the authors. </li> </ul>
Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
<p>This data set consists of 1D radiative-convective equilibrium boundary conditions for Jupiter-like giant planets, computed using coolTLUSTY and a recently updated set of molecular absorption cross sections. Models span internal temperatures of 80 - 450 K, and surface gravities of log10(g / [cm/s^2]) = 1.8 - 3.6. The planet is irradiated by a black body star at a distance of 5.2AU with effective temperature of 5777K with the zenith angle factor (accounting for an average incident angle) being FACFLX=0.5 or 0.67. The models assume a composition of 3.16x solar abundance, and allow the formation of ammonia clouds at low temperatures with characteristic sizes of 1 or 3 micron. More numerical details on the treatments of irradiation and clouds can be found in "Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations", arXiv number TBA.</p> <p>See README.txt for a description of data formats.</p>
Microlensing events indicate that super-Earth exoplanets are common in Jupiter-like orbits
Open the record for dataset details and reuse information.
Reinflation of Warm and Hot Jupiters
<p>This dataset contains the necessary inlists and other input files to reproduce the results of Komacek, Thorngren, Lopez, & Ginzburg (2020), "Re-inflation of warm and hot Jupiters" (<a href="https://ui.adsabs.harvard.edu/abs/2020ApJ...893...36K/abstract">https://ui.adsabs.harvard.edu/abs/2020ApJ...893...36K/abstract</a>). </p>
The_Global_Distribution_of_Ultra-Low-Frequency_Waves_in_Jupiter's_Magnetosphere_MannersH_ds01
<p>A supporting information dataset for the article "The Global Distribution of Ultra-Low-Frequency Waves in Jupiter's Magnetosphere", submitted by H. Manners and A. Masters. The file contains an Excel spreadsheet detailing the "datetime" intervals containing the events used in the survey described by the article. Additional details are listed alongside the datetimes: the average positions of the spacecraft during each event in radius from the planet, latitude and local time, expressed in Sysem III Jovian coordinates.</p>
Low-Latitude Whistler-Mode and Higher-Latitude Z-mode Emission at Jupiter Observed by Juno
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2020JA028742">10.1029/2020JA028742</a></p> <p><strong>Abstract</strong></p> <p>Whistler-mode chorus emission is important in the scattering and acceleration of electrons and filling of the radiation belts at Jupiter. In this work whistler mode magnetic intensity levels at Jupiter are comprehensively binned and parameterized. The frequency range of whistler mode under study extends from the proton cyclotron frequency, f<sub>cH</sub>, to f<sub>ceq</sub>/2, where f<sub>ceq</sub> is the cyclotron frequency mapped to the magnetic equator. Parametric dependence of magnetic plasma wave intensity is obtained versus frequency, latitude, and M-shell, as determined using a current magnetic field model based on Juno data. The results extend similar analyses of Jupiter whistler-mode emission obtained by the Galileo spacecraft, particularly on the nightside, and provide better coverage in latitude. Peaks in whistler-mode emission occur near M ~ 8-9, similar to previous studies, with average peak intensities approaching 10<sup>-2</sup> nT<sup>2</sup>, as also found by Galileo on the dayside. Auroral hiss and probably Z-mode are observed at higher latitudes. Jovian chorus emissions near an equatorial source region are more broad-banded than terrestrial chorus, and are coincident with a broad-banded electron distribution of free energy and strong electron scattering to large pitch angles. Intense whistler mode within a young plasma injection region is also observed, similar to injections in Saturn's magnetosphere. Future study of wave particle interactions within the chorus source region will be important. Possible Z-mode emission at significant intensity levels is observed in Jupiter’s inner magnetosphere, more intense, but not unlike Z-mode observed at Saturn.</p> <p><strong>Key Points</strong></p> <ul> <li>Jupiter whistler-mode & Z-mode intensity is binned in f, M, Magnetic latitude, and MLT</li> <li>Chorus emission coincident with electron scattering in source region</li> <li>Narrowband Z-mode emission likely observed at higher frequencies</li> </ul>
The High-Latitude Extension of Jupiter's Io Torus: Electron Densities Measured by Juno Waves
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2021JA029195">10.1029/2021JA029195</a></p> <p><strong>Abstract</strong></p> <p>We present Jovian electron densities measured by the Juno Waves instrument at high-latitudes on magnetic field lines threading the Io torus using the first 29 orbits of the Juno mission. We infer electron densities from characteristic frequency cutoffs and resonances in plasma wave spectra. There are often times when more than one of the characteristic frequency of the plasma can be identified, whose consistency provides more credibility to the plasma density estimates. The majority of density measurements are on magnetic field lines threading the Io torus and intersecting Jupiter's ionosphere between Io's M-shell and the auroral main oval, but there is evidence of density dropouts near and within the auroral oval, which may be important in auroral particle acceleration. Sharp density gradients are found near the inner edge of the Io torus region. These observations demonstrate the extension of elevated Io torus densities along field lines to higher latitudes. </p> <p><strong>Key Points</strong></p> <ul> <li>We present Jovian electron densities at high-latitudes on magnetic field lines connected to the Io torus and plasma sheet</li> <li>Sharp density gradients are found near the inner edge of the Io torus M-shell</li> <li>Our densities are consistent with partial electron densities measured by Juno's Jovian Auroral Distributions Experiment</li> </ul>
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