gas giant Archives

The radial gas temperature maps of planets from the 3D AFGKM ExoRad with a global temperature, Tglobal of 800K (left), 1600K (center) and 2400K (right) that orbit different host stars (top to bottom: A, G, M). The (Tgas, pgas)-maps gas are shown as equatorial slice plots. -- astro-ph.EP

AI - Data - Apps - Cybernetics, Atmospheres, Climate, Weather, Exoplanets, -moons, -comets, Gas Giants, Status Report

Accelerating Exoplanet Climate Modelling: A Machine Learning Approach To Complement 3D GCM Grid Simulations

by Keith CowingAugust 15, 2025August 15, 2025

With the development of ever-improving telescopes capable of observing exoplanet atmospheres in greater detail and number, there is a growing demand for enhanced 3D climate models to support and help […]

Global atmospheric C/O values for directly-imaged (blue) and transiting (purple) planets as a function of semi-major axis (left) and planet mass (right). This plot is reproduced using the data compiled in Hoch et al. (2023). Added to this plot are values from current C/O values reported in the literature (Ahrer et al. 2023; Alderson et al. 2023; Feinstein et al. 2023; Rustamkulov et al. 2023; Tsai et al. 2023; Edwards & Changeat 2024; Smith et al. 2024; Xue et al. 2024; Bell et al. 2023; Radica et al. 2023; Taylor et al. 2023; Coulombe et al. 2023) from the analysis (or inclusion) of data from JWST (orange). Error bars are included only if reported. The dotted horizontal line shows the solar C/O value (0.58; Asplund et al. 2021). -- astro-ph.EP

Astrochemistry, Astrogeology, Biogeochemical Cycles & Geobiology, Exoplanets, -moons, -comets, Gas Giants, Icy Worlds, Status Report

Linking Planet Formation To Exoplanet Characteristics: C/O As A Diagnostic Of Planet Formation

by Keith CowingAugust 14, 2025August 14, 2025

Gas-giant exoplanets are test cases for theories of planet formation as their atmospheres are proposed to carry signatures of their formation within the protoplanetary disk.

Maximum predicted emission frequency and radio flux density for known exoplanets (triangle symbols; data from [8]). The uncertainties on the predictions are estimated to one order of magnitude for the flux density and a factor of 2-3 for the emission frequency12. The sensitivities for the ground-based (UTR-2, LOFAR, NenuFAR, SKA-Low, VLA, GMRT) and space-based (FARSIDE, LCRT, FARVIEW ) radio telescopes are labeled (for 10 min of integration time and a bandwidth of 24 MHz). The FARVIEW and LCRT sensitivity curves are taken from [19] and [2], respectively. The LuSEE-Night sensitivity curve is averaged over the entire two-year mission and includes post-processing using a LombScargle periodogram (see text for details). The possible detection of τ Boo b from LOFAR23 is shown as a red star. This figure is adapted from [9]. -- astro-ph.IM

Astronomy & Telescopes, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Magnetic Fields, Electromagnetism, bioelectricity,, Status Report

Studying Exoplanets In The Radio From The Moon

by Keith CowingAugust 14, 2025August 14, 2025

Exoplanets with and without a magnetic field are predicted to form, behave, and evolve very differently.

Comparison of the Kepler-90 system (gray) with our own solar system (blue). The size of each circle is proportional to the planet’s radius. Masses for the inner six Kepler-90 planets are estimated using their measured radii and an empirical mass-radius relation (Weiss & Marcy 2014). Error bars are generally too small to be seen on this scale. Lines of constant RV semi-amplitude are drawn for a solar-mass star and circular orbit to approximately illustrate the RV signal induced by each planet. astro-ph.EP

Astronomy & Telescopes, Exoplanets, -moons, -comets, Gas Giants, Status Report

Updated Masses for the Gas Giants in the Eight-Planet Kepler-90 System Via Transit-Timing Variation and Radial Velocity Observations

by Keith CowingJuly 24, 2025July 24, 2025

The eight-planet Kepler-90 system exhibits the greatest multiplicity of planets found to date. All eight planets are transiting and were discovered in photometry from the NASA Kepler primary mission.

Left: Planet-to-star mass ratio as a function of the planet semi-major axis for all planets orbiting M-dwarf stars. Darker coloured symbols correspond to planetary masses above 0.2 MJup. Horizontal dotted lines indicate the Jupiter-to-Sun and Saturn-to-Sun mass ratios for reference. Right: Host star metallicity as a function of the insolation at the exoplanet semi-major axis. For multi-planetary systems, only the innermost planet is depicted. Vertical dotted lines indicate current insolation values of Jupiter and Saturn for reference. In both panels, different detection techniques are shown as labelled. Star symbols depict planets in the CARMENES sample (filled symbols, this work, and empty symbols, Trifonov et al. 2018, 2020a; Quirrenbach et al. 2022). -- astro-ph.EP

Astrogeology, Astronomy & Telescopes, Exoplanets, -moons, -comets, Gas Giants, Imaging & Spectroscopy, Status Report

The CARMENES Search For Exoplanets Around M Dwarfs. Revisiting The GJ 317, GJ 463, and GJ 3512 Systems And Two Newly Discovered Planets Orbiting GJ 9773 And GJ 508.2

by Keith CowingJuly 22, 2025July 22, 2025

Surveys for exoplanets indicate that the occurrence rate of gas giant planets orbiting late-type stars in orbits with periods shorter than 1000 days is lower than in the case of […]

The 134Xe/132Xe versus 136Xe/132Xe diagram showing the composition of Tatahouine (#13349) and Shalka (#6766 C) measured at different heating steps, including those of Michel & Eugster (1994) and Eugster & Michel (1995) for comparison. The 238U and 244Pu fission Xe data are from Porcelli et al. (2002). Q-Xe (Q phase is the main carrier of heavy noble gases in chondrites) is from Busemann et al. (2000), SW-Xe (SW stands for solar wind) is from Meshik et al. (2020), U-Xe is from Pepin & Porcelli (2002) and Air (corresponding to Earth’s atmosphere) -- astro-ph.EP

Astrochemistry, Astrogeology, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Comets and Asteroids, Gas Giants, Meteorites & Asteroids, Status Report

Asteroids Fail To Retain Cometary Impact Signatures

by Keith CowingJuly 3, 2025July 3, 2025

A bombardment of comets is thought to have occurred in the inner solar system as a result of a dynamical instability among the giant planets after gas disk dispersal.

Planetary growth timescales in an irradiated disc

Exoplanets, -moons, -comets, Gas Giants, Ice Giant, Icy Worlds, Status Report

Super-Earth Formation In Systems With Cold Giants

by Keith CowingJune 29, 2025June 28, 2025

Around our Sun, terrestrial planets did not grow beyond Earth in mass, while super-Earths are found to orbit approximately every other solar-like star.

Mass-Radius plot of asteroids, moons, planets, brown dwarfs and low-mass stars. From nearly 5600 exoplanets listed in the PHL-HWC database, 1504 are categorized as terrestrial worlds (orange dots), 2609 as Neptunian worlds (green dots), 1355 as Jovian worlds (purple dots), and 115 as brown dwarfs (brown dots). -- astro-ph.EP

Astrogeology, Atmospheres, Climate, Weather, Brown Dwarfs, Exoplanets, -moons, -comets, Gas Giants, Ice Giant, Nomenclature, Systematics, Natural History, Status Report

(Re)-Defining Planets — the Fundamental Plane of Planets

by Keith CowingJune 23, 2025June 23, 2025

6000+ exoplanets are now detected using various techniques, with estimates of billions of planets existing in our Galaxy alone.

Binary collision-induced H2–He absorption coefficient, α, normalized by the hydrogen and helium gas densities, as function of frequency in the fundamental band, at 296 K. The parato-ortho distribution, is representative of equilibrium H2, just as in Fig. 2. Our model (“this work”), is compared with the model of Abel et al.17 for T = 300K, and with the laboratory measurements of Vitali et al. 18 and Brodbeck et al.19 , both of which were made near 296 K. We note that neither our model nor that of Abel et al. considered the discrete, intercollisional interference dips present in the laboratory spectra. -- astro-ph.EP

Atmospheres, Climate, Weather, Exoplanets, -moons, -comets, Gas Giants, Ice Giant, Jupiter, Neptune, Saturn, Status Report, Uranus

Improved H2-He and H2-H2 Collision-Induced Absorption Models and Application to Outer-Planet Atmospheres

by Keith CowingJune 15, 2025June 13, 2025

Using state-of-the-art ab initio interaction-induced dipole and potential-energy surfaces for hydrogen-helium (H2-He) pairs, we compute the rototranslational collision-induced absorption coefficient at 40-400 K for frequencies covering 0-4000 cm-1.

First direct image of 14 Her c. JWST/NIRCam coronagraphic imaging of the 14 Her system with the MASKA335R coronagraph (transmission indicated by gray shaded circles). North is up, east is left. Left: Prediction for the location of 14 Her c from a reproduction of the orbits presented in (G. F. Benedict et al. 2023), at the epoch of observation (MJD=60449), and the location of the point source detected in the F444W filter. Middle: A starlight-subtracted image taken with the F200W filter (1.755−2.227 µm), showing extended emission from a background galaxy at about 1. ′′5 to the SE from the host star. No other statistically significant point sources are apparent, as intended, given the cold temperature of the planet 14 Her c. Right: A starlight-subtracted image taken with the F444W filter (3.881−4.982 µm), showing extended emission from the same background galaxy, and a point source at 1. ′′1 to the SW with a contrast of 1 × 10−6 . The location of the point source, detected with a contrast of 9.6 × 10−7 , agrees within 1σ with the predicted location for the planet, so we conclude we have detected 14 Her c. -- (astro-ph.EP

Astronomy & Telescopes, Exoplanets, -moons, -comets, Gas Giants, Status Report

JWST Coronagraphic Images of 14 Her c: a Cold Giant Planet in a Dynamically Hot, Multi-planet System

by Keith CowingJune 14, 2025June 12, 2025

Most observed multi-planet systems are coplanar, in a dynamically “cold” configuration of concentric orbits like our own Solar System.

gas giant

Accelerating Exoplanet Climate Modelling: A Machine Learning Approach To Complement 3D GCM Grid Simulations

Linking Planet Formation To Exoplanet Characteristics: C/O As A Diagnostic Of Planet Formation

Studying Exoplanets In The Radio From The Moon

Updated Masses for the Gas Giants in the Eight-Planet Kepler-90 System Via Transit-Timing Variation and Radial Velocity Observations

The CARMENES Search For Exoplanets Around M Dwarfs. Revisiting The GJ 317, GJ 463, and GJ 3512 Systems And Two Newly Discovered Planets Orbiting GJ 9773 And GJ 508.2

Asteroids Fail To Retain Cometary Impact Signatures

Super-Earth Formation In Systems With Cold Giants

(Re)-Defining Planets — the Fundamental Plane of Planets

Improved H2-He and H2-H2 Collision-Induced Absorption Models and Application to Outer-Planet Atmospheres

JWST Coronagraphic Images of 14 Her c: a Cold Giant Planet in a Dynamically Hot, Multi-planet System

NASA Planetary Protection Handbook

NASA Scientists Search For Clues About Mars’ Past In Scotland

A Temperate Sub-Neptune Transiting The M4 Dwarf TOI-210 Identified By NIRPS And TESS — Uncovering Hidden M-dwarf Planetary Systems In The Near-infrared

Nonequilibrium Formation of Pyridine (C5H5N) in Interstellar Ice Analogs: Implications for Biorelevant Nitrogen Heterocycles in Ryugu and Bennu

The Abundance And Emission Of PAHs From The Local To Early Universe