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SUMMARY:Most Rocky Sub-Neptunes are Molten: Mapping the Solidification Sho
 reline for Gas Dwarf Exoplanets - Robb Calder (Cambridge)
DTSTART:20251202T130000Z
DTEND:20251202T140000Z
UID:TALK240214@talks.cam.ac.uk
CONTACT:James Rogers
DESCRIPTION:Sub-Neptunes are the most common type of detected exoplanet\, 
 yet their observed masses and radii are degenerate with several interior s
 tructures. One possibility is that sub-Neptunes have silicate/iron interio
 rs and H2-dominated atmospheres\, i.e.\, they are `Gas Dwarfs'. If gas dwa
 rfs have fully molten interiors\, interactions between their magma oceans 
 and atmospheres would produce distinct observational signatures. These sig
 natures may break the degeneracy in interior structure. We use the coupled
  interior-climate evolution model\, PROTEUS\, to estimate the 'solidificat
 ion shoreline': the instellation flux boundary that separates molten gas d
 warfs from solidified ones. Our results show that 98% of detected sub-Nept
 unes occupy a region of parameter space consistent with their having perma
 nent magma oceans. Therefore\, most detected sub-Neptunes (if they are gas
  dwarfs) have permanent magma oceans. This result motivates further resear
 ch into the interactions between molten interiors and overlying atmosphere
 s.
LOCATION:Ryle seminar room + ONLINE - Details to be sent by email
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