Study Findings: A Second Visit to Eps Ind Ab with JWST: New Photometry Confirms Ammonia and Suggests Thick Clouds in the Exoplanet Atmosphere of the Closest Super-Jupiter

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Image (Credit): Juno mission image of Jupiter taken on Juno’s 22nd close pass by Jupiter on Sept. 12, 2019. (NASA/JPL-Caltech/SwRI/MSSS / Image processing by Prateek Sarpal, © CC NC SA)

The Astrophysical Journal Letters abstract of study findings:

With JWST, we are directly imaging cold (∼200–300 K) solar-age giant exoplanets for the first time. At these temperatures, many molecular features appear, and water-ice clouds may condense and affect the emission spectrum; early photometric measurements of cold giant planets are already showing some tension with the predictions of cloud-free solar-metallicity atmosphere models. Here, we present new JWST/MIRI coronagraphic observations of the cold giant exoplanet Eps Ind Ab at 11.3 μm. Together with archival data, we use these new observations to study the atmosphere of this cold exoplanet, and we also refit its orbit, finding an updated mass of 7.6  ±  0.7MJup and an eccentricity of 0.24 +0.11/-0.08. The planet is significantly brighter (by 0.88  ±  0.08 mag) at 11.3 μm than at 10.6 μm, indicating the presence of ammonia. However, this ammonia feature is shallower than expected. This could indicate a low-metallicity or nitrogen-depleted atmosphere, but our preferred explanation is the presence of thick water-ice clouds that suppress the ammonia feature and the near-IR emission of Eps Ind Ab. Photometry of the small but growing sample of cold giant exoplanets demonstrates that they are consistently fainter than expected between 3 and 5 μm, consistent with the water-ice cloud hypothesis. 10.6 μm and 11.3 μm photometry of this cold exoplanet sample would be valuable to determine whether the suppressed ammonia feature is universal, and to frame a new open question about the underlying physical cause.

Citation: Elisabeth C. Matthews et al. a second visit to eps ind ab with JWST: new photometry confirms ammonia and suggests thick clouds in the exoplanet atmosphere of the closest super-Jupiter, ApJL 1002 L5 (2026).

DOI: 10.3847/2041-8213/ae5823

Study-related stories:

Max Planck Institute for Astronomy – “Cirrus Clouds Made of Water Ice May Surround a Jupiter-like Exoplanet”

Universe Today – “Webb Finds Water-Ice Clouds on Nearby Super-Jupiter”

Sci.News – “Webb Spots Icy Clouds on Distant Jupiter-Like Exoplane”

Study Findings: An Adolescent and Near-resonant Planetary System Near the End of Photoevaporation

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Credit: Image by Adis Resic from Pixabay

Nature Astronomy abstract of study findings:

Young exoplanets provide vital insights into the early dynamical and atmospheric evolution of planetary systems. Many multi-planet systems younger than 100 Myr exhibit mean-motion resonances, probably established through convergent disk migration. Over time, however, these resonant chains are often disrupted, mirroring the Nice model proposed for the Solar System. Here we present a detailed characterization of the ~200-Myr-old TOI-2076 system, which contains four sub-Neptune planets between 1.4 and 3.5 Earth radii. We demonstrate that its planets are near to but not locked in mean-motion resonances, making the system dynamically fragile. The four planets have comparable core masses but display a monotonic increase in hydrogen and helium (H/He) envelope mass fractions (from stripped to 1%, 5% and 5%) with decreasing stellar insolation. This trend is consistent with atmospheric mass loss due to photoevaporation, which predicts that the envelopes of irradiated planets either erode completely or stabilize at a residual level of ~1% by mass within the first few hundred million years, with more distant, less-irradiated planets retaining most of their primordial envelopes. Additionally, previous detections of metastable helium outflows rule out a pure water-world scenario for the TOI-2076 planets. Our finding provides direct observational evidence that the dynamical and atmospheric reshaping of compact planetary systems begins early and offers an empirical anchor for models of their long-term evolution.

Citation: Wang, MT., Dai, F., Liu, HG. et al. An adolescent and near-resonant planetary system near the end of photoevaporation, Nat Astron (2026).

https://doi.org/10.1038/s41550-026-02795-9

Study-related stories:

Florida Tech – “Assessment of Rare Teenage Planetary System Deepens Understanding of Cosmic Evolution”

Universe Today – “Adolescence Is Tumultuous, Even For Exoplanets”

Daily Galaxy – “Scientists Discover ‘Teenage’ Planetary System, Unlocking Secrets of Cosmic Growth”

Study Findings: Building Wet Planets Through High-Pressure Magma–Hydrogen Reactions

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Credit: Image by Yol Gezer from Pixabay

Nature abstract of study findings:

Close-in transiting sub-Neptunes are abundant in our Galaxy. Planetary interior models based on their observed radius–mass relationship suggest that sub-Neptunes contain a discernible amount of either hydrogen (dry planets) or water (wet planets) blanketing a core composed of rocks and metal. Water-rich sub-Neptunes have been believed to form farther from the star and then migrate inwards to their present orbits. Here we report experimental evidence of reactions between warm, dense hydrogen fluid and silicate melt that release silicon from the magma to form alloys and hydrides at high pressures. We found that oxygen liberated from the silicate melt reacts with hydrogen, producing an appreciable amount of water up to a few tens of weight per cent, which is much greater than previously predicted based on low-pressure ideal gas extrapolation. Consequently, these reactions can generate a spectrum of water contents in hydrogen-rich planets, with the potential to reach water-rich compositions for some sub-Neptunes, implying an evolutionary relationship between hydrogen-rich and water-rich planets. Therefore, detection of a large amount of water in exoplanet atmospheres may not be the optimal evidence for planet migration in the protoplanetary disk, calling into question the assumed link between composition and planet formation location.

Citation: Horn, H.W., Vazan, A., Chariton, S. et al. Building wet planets through high-pressure magma–hydrogen reactions. Nature 646, 1069–1074 (2025).

https://doi.org/10.1038/s41586-025-09630-7

Study-related stories:

Science News – “Some Planets Might Home Brew their Own Water”

Universe Today – “Some Exoplanets Can Create Their Own Water Through Crust-Atmosphere Reactions”

Space Daily – “Water Production on Exoplanets Revealed by Pressure Experiments”

Pic of the Week: Another View of the Milky Way

Posted on by onespaceman2000
Image (Credit): The Milky Way galaxy in radio waves as seen from the Southern Hemisphere. (Silvia Mantovanini and the GLEAM-X Team)

The image above was released late last year. It shows the Milky Way galaxy in radio-color captured by astronomers from the International Centre of Radio Astronomy Research (ICRAR). All of this was part of the GaLactic and Extragalactic All-sky MWA (GLEAM) and GLEAM-X (GLEAM eXtended) surveys conducted over 28 nights in 2013 and 2014 as well as 113 nights from 2018 to 2020.

In describing the image, Silvia Mantovanini, one of the astronomers analyzing the survey data, noted:

You can clearly identify remnants of exploded stars, represented by large red circles. The smaller blue regions indicate stellar nurseries where new stars are actively forming.

In this video, you can hear more from astronomers Silvia Mantovanini and Natasha Hurley-Walker who co-wrote a paper on this work titled GaLactic and extragalactic all-sky Murchison Widefield Array survey eXtended (GLEAM-X) III: Galactic plane.

Study Findings: A Binary Model of Long-Period Radio Transients and White Dwarf Pulsars

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Credit: Casey Reed, NASA

Nature Astronomy abstract of study findings:

Long-period radio transients (LPTs) represent a recently uncovered class of Galactic radio sources exhibiting minutes to hours periodicities and highly polarized pulses of seconds to minutes duration. Their phenomenology does not fit exactly in any other class, although it might resemble that of radio magnetars or white dwarf (WD) pulsars. Two LPTs with confirmed multi-wavelength counterparts have now been identified as WD – M dwarf binaries. Moreover, WD pulsars (also WD – M dwarf systems), such as AR Scorpii and J1912−44, are known to exhibit short-period pulsations in hour-timescale orbits. Here we investigate the longest-lived LPT known, GPM J1839−10. We use a 36-year timing baseline to infer an ~8.75-h orbital period from radio data alone, and we show that it can be modelled in the same geometric framework as has been proposed for WD pulsars. Radio emission is triggered when the magnetic axis of a rotating WD intersects the wind from its companion, which naturally predicts the peculiar pulse modulation. Applying this to the WD pulsar J1912−44 successfully reproduces the emission profile and geometry as well. Our results indicate analogous emission-site geometries in these related classes of binary system, a possibility we extend to the broader LPT and WD pulsar population.

Citation: Horváth, C., Rea, N., Hurley-Walker, N. et al. A binary model of long-period radio transients and white dwarf pulsars. Nat Astron (2026).

https://doi.org/10.1038/s41550-025-02760-y

Study-related stories:

The Conversation – “Puzzling Slow Radio Pulses are Coming from Space. A New Study Could Finally Explain Them”

The Institute of Space Studies of Catalonia – “A Binary Star System Explains Mysterious Radio Pulses Across the Milky Way”

Sci.News – “Sporadic Radio Pulses Traced to White Dwarf-Red-Dwarf Binary System”