A warm Neptune’s methane reveals core mass and vigorous atmospheric mixing (2024)

Abstract

Observations of transiting gas giant exoplanets have revealed a pervasive depletion of methane1,2,3,4, which has only recently been identified atmospherically5,6. The depletion is thought to be maintained by disequilibrium processes such as photochemistry or mixing from a hotter interior7,8,9. However, the interiors are largely unconstrained along with the vertical mixing strength and only upper limits on the CH4 depletion have been available. The warm Neptune WASP-107 b stands out among exoplanets with an unusually low density, reported low core mass10, and temperatures amenable to CH4 though previous observations have yet to find the molecule2,4. Here we present a JWST NIRSpec transmission spectrum of WASP-107 b which shows features from both SO2 and CH4 along with H2O, CO2, and CO. We detect methane with 4.2σ significance at an abundance of 1.0±0.5 ppm, which is depleted by 3 orders of magnitude relative to equilibrium expectations. Our results are highly constraining for the atmosphere and interior, which indicate the envelope has a super-solar metallicity of 43±8× solar, a hot interior with an intrinsic temperature of Tint=460±40 K, and vigorous vertical mixing which depletes CH4 with a diffusion coefficient of Kzz = 1011.6±0.1 cm2/s. Photochemistry has a negligible effect on the CH4 abundance, but is needed to account for the SO2. We infer a core mass of \({{\boldsymbol{11.5}}}_{-{\boldsymbol{3.6}}}^{+{\boldsymbol{3.0}}}\) M, which is much higher than previous upper limits10, releasing a tension with core-accretion models11.

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Authors and Affiliations

  1. Department of Earth & Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA

    David K. Sing&Zafar Rustamkulov

  2. Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA

    David K. Sing,Daniel P. Thorngren&Elena Manjavacas

  3. School of Physical Sciences, The Open University, Milton Keynes, UK

    Joanna K. Barstow

  4. Université Paris-Saclay, UVSQ, CNRS, CEA, Maison de la Simulation, Gif-sur-Yvette, France

    Pascal Tremblin

  5. Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France

    Pascal Tremblin

  6. European Space Agency, European Space Astronomy Centre, 28692 Villanueva de la Canada, Madrid, Spain

    Catarina Alves de Oliveira,Stephan M. Birkmann&Pierre Ferruit

  7. Space Telescope Science Institute, Baltimore, MD, USA

    Tracy L. Beck,Néstor Espinoza,Amélie Gressier&Jeff A. Valenti

  8. Department of Astronomy and Carl Sagan Institute, Cornell University, Ithaca, NY, USA

    Ryan C. Challener&Nikole K. Lewis

  9. Leiden Observatory, Leiden University, P.O. Box 9513, Leiden, The Netherlands

    Nicolas Crouzet

  10. ATG Europe for the European Space Agency, ESTEC, Noordwijk, The Netherlands

    Giovanna Giardino

  11. Center for Space and Habitability, University of Bern, Bern, Switzerland

    Elspeth K. H. Lee

  12. University of Cambridge, The Old Schools, Trinity Ln, Cambridge, UK

    Roberto Maiolino

  13. AURA for the European Space Agency (ESA), ESA Office, Space Telescope Science Institute, Baltimore, MD, USA

    Elena Manjavacas

  14. NASA Goddard Space Flight Center, Greenbelt, MD, USA

    Bernard J. Rauscher

  15. European Space Agency (ESA), ESA Office, Space Telescope Science Institute, Baltimore, MD, USA

    Marco Sirianni

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  1. David K. Sing

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  2. Zafar Rustamkulov

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  3. Daniel P. Thorngren

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  4. Joanna K. Barstow

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  6. Catarina Alves de Oliveira

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  11. Néstor Espinoza

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  15. Elspeth K. H. Lee

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  16. Nikole K. Lewis

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  17. Roberto Maiolino

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  18. Elena Manjavacas

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  20. Marco Sirianni

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  21. Jeff A. Valenti

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Correspondence to David K. Sing.

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A warm Neptune’s methane reveals core mass and vigorous atmospheric mixing (4)

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Sing, D.K., Rustamkulov, Z., Thorngren, D.P. et al. A warm Neptune’s methane reveals core mass and vigorous atmospheric mixing. Nature (2024). https://doi.org/10.1038/s41586-024-07395-z

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A warm Neptune’s methane reveals core mass and vigorous atmospheric mixing (2024)

FAQs

Why does methane make Neptune blue? ›

Neptune's atmosphere is made up of hydrogen, helium and methane. The methane in Neptune's upper atmosphere absorbs the red light from the sun but reflects the blue light from the Sun back into space. This is why Neptune appears blue.

What is Neptune's atmosphere composed of? ›

Neptune's atmosphere is made up mostly of hydrogen and helium with just a little bit of methane.

Does Neptune have a solid core? ›

Like the other giant planets in our solar system, Neptune does not have a solid surface. Scientists believe that the interior of the planet is made up of a solid rocky core covered by a hot and dense liquid layer of water and ammonia.

What gas is surrounding Neptune? ›

Like the gas giants (Jupiter and Saturn), Neptune's atmosphere is composed primarily of hydrogen and helium, along with traces of hydrocarbons and possibly nitrogen, but contains a higher proportion of ices such as water, ammonia and methane.

What makes Neptune look so blue? ›

Sunlight is therefore reflected back into space, not by a solid surface as with Earth, but by gases in Neptune's atmosphere. These gases are dominated by hydrogen and helium with a smaller amount of methane and it is the methane that is responsible for Neptune's colour - methane absorbs red light and reflects blue.

Why does methane reflect blue light? ›

Methane absorbs red light and reflects blue, which is why both planets have a generally blue color. There are traces of other elements in their atmospheres, and the chemical reactions between various molecules can create a haze of aerosols that can taint their basic blue hue.

What is Neptune's core made of? ›

Like Earth, Neptune has a rocky core made up of iron and other metals, with a mass just greater than our planet. Temperatures in the core could reach 9,260 F (5,127 C). Like the other gas giants, Neptune boasts a series of rings.

How much methane is on Neptune? ›

atmosphere contains ~80% hydrogen, 19% helium, and 1.5% methane.

Is Neptune drifting away? ›

No, Neptune is not moving away from the solar system. In fact, all the planets in our solar system, including Neptune, are in stable orbits around the Sun. This is due to the balance between the gravitational forces that pull the planets towards the Sun and the centrifugal forces that push them outwards.

Does Diamond Rain on Neptune? ›

In addition to these directly observable characteristics, at the immense pressures inside these giants, familiar materials can transform into exotic forms. One possible phenomenon is particularly dazzling: deep within Neptune and Uranus, it may rain diamonds.

Can you stand on Neptune's core? ›

If a person were to attempt to stand on Neptune, they would sink through the gaseous layers. As they descended, they would experience increased temperatures and pressures until they finally touched down on the solid core itself.

Can humans go to Pluto? ›

“But it would be premature to send human beings to most places in the solar system, including Pluto, today, because we don't know enough about the planet to design such a mission. It's also very far beyond our technical capabilities, and there's no present need to spend the kind of money that it would take.

What planet has the most beautiful rings? ›

No other planet in our solar system has rings as splendid as Saturn's. They are so expansive and bright that they were discovered as soon as humans began pointing telescopes at the night sky.

What planet rotates backwards compared to Earth? ›

Yes, Venus spins backwards compared to most of the other planets. It spins or rotates in the opposite direction that Earth rotates. This means that on Venus the Sun rises in the west and sets in the east.

What planet has the fastest revolution? ›

Mercury is the fastest orbiting planet of our solar system.

Does methane make the sky blue? ›

The blue of the sky is primarily due scattering by gas molecules that are mostly nitrogen (~78%) and oxygen (~20%) plus a number of other gases ( e.g., carbon dioxide, methane, ozone). The small size of these molecules scatters primarily the blue component of sunlight.

Why do Uranus and Neptune have blue methane clouds? ›

In this layer on both planets, methane ice condenses on aerosols, but then the two worlds diverge. Neptune's more active atmosphere likely produces snow as it moves methane particles into the haze, which removes haze over time. Uranus, however, has a thicker layer of haze due to its slower-moving atmosphere.

Why does methane in the atmosphere cause Uranus to look blue-green? ›

Uranus gets its blue-green color from methane gas in the atmosphere. Sunlight passes through the atmosphere and is reflected back out by Uranus' cloud tops. Methane gas absorbs the red portion of the light, resulting in a blue-green color.

What two gas giants appear blue because of the methane? ›

Neptune and Uranus look blue/green due to methane in their atmosphere. Mercury and Mars look red due to red rocks on their surface.

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