Planetary Climate Dynamics

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The JWST weather report from the nearest brown dwarfs I: multiperiod JWST NIRSpec + MIRI monitoring of the benchmark binary brown dwarf WISE 1049AB

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 532:2 (2024) 2207-2233

Authors:

Beth A Biller, Johanna M Vos, Yifan Zhou, Allison M McCarthy, Xianyu Tan, Ian JM Crossfield, Niall Whiteford, Genaro Suarez, Jacqueline Faherty, Elena Manjavacas, Xueqing Chen, Pengyu Liu, Ben J Sutlieff, Mary Anne Limbach, Paul Molliere, Trent J Dupuy, Natalia Oliveros-Gomez, Philip S Muirhead, Thomas Henning, Gregory Mace, Nicolas Crouzet, Theodora Karalidi, Caroline V Morley, Pascal Tremblin, Tiffany Kataria
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Mapping the transition from liquid to supercritical water on sub-Neptunes

Copernicus Publications (2024)

Authors:

Hamish Innes, Raymond Pierrehumbert
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From stars to diverse mantles, melts, crusts and atmospheres of rocky exoplanets

Reviews in Mineralogy and Geochemistry 90 (2024)

Authors:

Claire Marie Guimond, Haiyang Wang, Fabian Seidler, Paolo Sossi, Aprajit Mahajan, Oliver Shorttle

Abstract:

This review is focused on describing the logic by which we make predictions of exoplanetary compositions and mineralogies, and how these processes could lead to compositional diversity among rocky exoplanets. We use these predictions to determine the sensitivity of present-day and future observations to detecting compositional differences between rocky exoplanets and the four terrestrial planets. First, we review data on stellar abundances and infer how changes in composition may manifest themselves in the expected bulk compositions of rocky exoplanets (section 2). Converting this information in mass-radius relationships requires calculation of the stable mineral assemblages at a given temperature-pressure-composition (T-P-X), an exercise we describe in section 3. Should the planet be hot enough to engender partial melting of the mantle, then these liquids are likely to rise to the surface and erupt to form planetary crusts; the possible compositional and mineralogical variability of which we examine in section 4. Finally, the expected spectroscopic responses of such crusts are examined in section 5.
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Direct detectability of tidally heated exomoons by photometric orbital modulation

Astronomy & Astrophysics EDP Sciences 687 (2024) a125

Authors:

E Kleisioti, D Dirkx, X Tan, MA Kenworthy
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Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS

Astronomical Journal IOP Publishing 168:1 (2024) 4

Authors:

Mark Hammond, Taylor J Bell, Ryan C Challener, Neil T Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L Bean, Ludmila Carone, João M Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C Nixon, Benjamin V Rackham, Jingxuan Yang

Abstract:

We present eclipse maps of the two-dimensional thermal emission from the dayside of the hot-Jupiter WASP-43b, derived from an observation of a phase curve with the JWST MIRI/LRS instrument. The observed eclipse shapes deviate significantly from those expected for a planet emitting uniformly over its surface. We fit a map to this deviation, constructed from spherical harmonics up to order ℓmax=2 , alongside the planetary, orbital, stellar, and systematic parameters. This yields a map with a meridionally averaged eastward hot-spot shift of (7.75 ± 0.36)°, with no significant degeneracy between the map and the additional parameters. We show the latitudinal and longitudinal contributions of the dayside emission structure to the eclipse shape, finding a latitudinal signal of ∼200 ppm and a longitudinal signal of ∼250 ppm. To investigate the sensitivity of the map to the method, we fix the parameters not used for mapping and derive an “eigenmap” fitted with an optimized number of orthogonal phase curves, which yields a similar map to the ℓmax=2 map. We also fit a map up to ℓmax=3 , which shows a smaller hot-spot shift, with a larger uncertainty. These maps are similar to those produced by atmospheric simulations. We conclude that there is a significant mapping signal which constrains the spherical harmonic components of our model up to ℓmax=2 . Alternative mapping models may derive different structures with smaller-scale features; we suggest that further observations of WASP-43b and other planets will drive the development of more robust methods and more accurate maps.
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