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DTSTART;TZID=America/Denver:20260609T110000
DTEND;TZID=America/Denver:20260609T120000
DTSTAMP:20260605T154857
CREATED:20260601T202830Z
LAST-MODIFIED:20260601T202830Z
UID:21931-1781002800-1781006400@www.boulder.swri.edu
SUMMARY:High energy planetary astrophysics: exomoons and their geological signatures in the magnetospheres of giant planets and dwarf stars
DESCRIPTION:Volcanic satellites — active moons orbiting giant planets\, or close-in active rocky planets orbiting dwarf stars — are among our best windows into geological activity beyond Earth. Even within our own solar system\, the 2014 claim of cryovolcanism at Jupiter’s satellite Europa has now been retracted (Roth et al. 2026)\, owing to the difficulty of inferring transient water vapor from low signal-to-noise aurorae. By contrast\, NaCl sourced from an evaporating or volcanically active ocean world such as Io or Enceladus provides one of the brightest available signatures\, namely in atomic sodium and potassium. Io ignites a sodium exosphere extending ~1000 Jupiter radii. Similar to the first radial-velocity detections of exoplanets\, we report the first Doppler shift of an exomoon system: an unambiguous redshift that\, in transmission geometry\, opposes the natural blueshift vector of radiation pressure (Oza et al. 2024\, ApJL). At the same system\, new KECK observations confirm a repeating ~40-minute transient sodium signature\, coincident with its Doppler shift\, first observed with HARPS/3.6-m (Unni et al. 2025\, MNRASL).  We characterize the orbit to be roughly 8 hours\, consistent with recent independent N-body simulations (Sucerquia & Cuello 2025\, A&A Letters). Without high-resolution spectroscopy \, JWST low-res spectroscopy cannot easily infer the periodicity of a satellite without a Doppler shift; nevertheless\, recent variability of SO₂ — a known volcanic gas — at WASP-39b\, seen by MIRI and NIRCam\, appears to require an exomoon and its associated plasma torus (8-15h orbit) rather than H₂S photochemistry of a planetary atmosphere alone (Oza et al. 2026\, MNRAS). Beyond optical/IR\, roughly a decade before the sodium cloud was detected at Io\, decametric radio emission at Jupiter notably provided the first evidence of Io’s volcanic escape (Bigg 1964). In this light\, we also report evidence of a volcanic satellite in a dwarf-star system based on its radio emission\, originally reported as a radiation belt (Kao et al. 2023).  Our modeling suggests a putative satellite is fueling the detected electron cyclotron maser instability (ECMI) observed as short bursts. Together\, these initial optical\, infrared\, and radio detections of active satellites opens a window onto planet–satellite formation and evolution\, informing the broader population of exomoons in the galaxy.
URL:https://www.boulder.swri.edu/event/high-energy-planetary-astrophysics-exomoons-and-their-geological-signatures-in-the-magnetospheres-of-giant-planets-and-dwarf-stars/
LOCATION:Conference Room 4.615
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/Denver:20260616T110000
DTEND;TZID=America/Denver:20260616T120000
DTSTAMP:20260605T154857
CREATED:20260407T233626Z
LAST-MODIFIED:20260527T230437Z
UID:21833-1781607600-1781611200@www.boulder.swri.edu
SUMMARY:Daniel Toledo - INTA - Madrid\, Deep NH₃/H₂S Composition and the Coupling of NH₄SH and H₂S Clouds in the Ice Giants
DESCRIPTION:Where: SwRI 4th Floor Seminar Room (white chairs)  + webex (see details below) \nDeep NH₃/H₂S Composition and the Coupling of NH₄SH and H₂S Clouds in the Ice Giants \nObservations of Uranus and Neptune indicate the presence of H₂S clouds at pressures greater than ~2 bar\, while thermochemical models predict the formation of NH₄SH clouds at deeper levels where NH₃ and H₂S react (~30–40 bar). The coupling between these cloud layers remains poorly understood\, despite its importance for interpreting the vertical structure and composition of giant planet atmospheres. \nIn this presentation\, we discuss results from an extended one-dimensional cloud microphysics model previously applied to simulate CH₄ and H₂S clouds in the Ice Giants. The model now incorporates NH₄SH chemistry\, extending the simulation domain to deeper atmospheric levels (~40 bar). Since NH₃ reacts with H₂S to form NH₄SH at depth\, the deep NH₃/H₂S ratio directly controls the amount of H₂S gas that can survive above the NH₄SH cloud layer and remain available to condense at higher altitudes. \nWe explore how the deep NH₃ and H₂S abundances\, together with the vertical mixing profile\, determine the properties of the observable H₂S cloud layer\, including its base pressure\, opacity\, and particle size distribution. Under Ice Giant conditions\, where deep H₂S abundances are expected to exceed those of NH₃\, the formation of a deep NH₄SH cloud can still significantly deplete the upward transport of sulfur-bearing gas\, indirectly modifying the structure of the upper H₂S cloud. \nFinally\, we discuss the contrasting regime expected in Jupiter and Saturn\, where NH₃ is likely more abundant than H₂S\, and how future observations\, particularly radiometric measurements\, could provide key constraints on the deep NH₃/H₂S composition through the study of cloud layers. \nLocation Details: \nHybrid – In person and Webex: \n4th floor conference room at SwRI Boulder:  (please see the 4th floor receptionist for a badge) \n1301 Walnut St. \nBoulder\, CO \n  \nWebex: https://swri15.webex.com/meet/ksinger \nPhone: 1-866-469-3239  Meeting Number: 2633 145 9127
URL:https://www.boulder.swri.edu/event/date-reserved-for-seminar-for-scot-rafkin/
LOCATION:Hybrid – In-person and Online – See details below the abstract
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/Denver:20260630T110000
DTEND;TZID=America/Denver:20260630T110000
DTSTAMP:20260605T154857
CREATED:20251126T170022Z
LAST-MODIFIED:20260507T183436Z
UID:21556-1782817200-1782817200@www.boulder.swri.edu
SUMMARY:Vertically Mapping the Cloud-Driven Atmospheric Dynamics & Chemistry of an Isolated Exoplanet Analog
DESCRIPTION:Young planetary-mass objects and brown dwarfs near the L/T spectral transition exhibit enhanced spectrophotometric variability over field brown dwarfs. Patchy clouds\, auroral processes\, stratospheric hot spots\, and complex carbon chemistry have all been proposed as potential sources of this variability. Using time-resolved\, low-to-mid-resolution spectroscopy collected with the JWST/NIRISS and NIRSpec instruments\, we apply harmonic analysis to SIMP J0136\, a highly variable\, young\, isolated planetary-mass object. Odd harmonics (k=3) at pressure levels (> 1 bar) corresponding to iron and forsterite cloud formation suggest North/South hemispheric asymmetry in the cloudy\, and likely equatorial\, regions. We use the inferred harmonics\, along with 1-D substellar atmospheric models\, to map the flux variability by atmospheric pressure level. These vertical maps demonstrate robust interaction between deep convective weather layers and the overlying stratified and radiative atmosphere. We identify distinct time-varying structures in the near-infrared that we interpret as planetary-scale wave (e.g.\, Rossby or Kelvin)-associated cloud modulation. We detect variability in water (S/N = 14.0)\, carbon monoxide (S/N = 13.0)\, and methane (S/N = 14.9) molecular signatures. Forsterite cloud modulation is anti-correlated with overlying carbon monoxide and water abundances and correlated with deep methane absorption\, suggesting complex interaction between cloud formation\, atmospheric chemistry\, and temperature structure. Furthermore\, we identify distinct harmonic behavior between methane and carbon monoxide absorption bands\, providing evidence for time-resolved disequilibrium carbon chemistry. At the lowest pressures (< 100 mbar)\, we find that the mapped methane lines transition from absorption to emission\, supporting evidence of high-altitude auroral heating via electron precipitation.
URL:https://www.boulder.swri.edu/event/tbd-6/
LOCATION:Conference Room 4.615
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/Denver:20260908T110000
DTEND;TZID=America/Denver:20260908T120000
DTSTAMP:20260605T154857
CREATED:20260415T192304Z
LAST-MODIFIED:20260506T001136Z
UID:21849-1788865200-1788868800@www.boulder.swri.edu
SUMMARY:Seminar- Abby Fraeman (JPL) - TBD Topic
DESCRIPTION:SwRI Seminar – Tuesday Sept 8 – Will be hybrid – Details TBD closer to the date!  (Contact Kelsi Singer for any questions)
URL:https://www.boulder.swri.edu/event/seminar-abby-fraeman-jpl-tbd-topic/
LOCATION:Hybrid – In-person and Online – See details below the abstract
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/Denver:20261201T110000
DTEND;TZID=America/Denver:20261201T120000
DTSTAMP:20260605T154857
CREATED:20260601T020023Z
LAST-MODIFIED:20260601T020149Z
UID:21923-1796122800-1796126400@www.boulder.swri.edu
SUMMARY:Seminar with Lauren Mc Keown (UCF) - Topic TBD
DESCRIPTION:TBD
URL:https://www.boulder.swri.edu/event/seminar-with-lauren-mc-keown-topic-tbd/
LOCATION:Hybrid – In-person and Online – See details below the abstract
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