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SUMMARY:Iron rain and iron snow in planetary interiors: insights from flui
 ds experiments - Dr Quentin Kriaa (University of Cambridge)
DTSTART:20260217T120000Z
DTEND:20260217T130000Z
UID:TALK242746@talks.cam.ac.uk
CONTACT:120229
DESCRIPTION:At a late stage of its accretion\, the Earth experienced high-
 energy planetary impacts. Following each collision\, the metal core of the
  impactor sank as millimetric drops into a molten silicate magma ocean —
  the so-called “iron rain”. The efficiency of chemical equilibration b
 etween metal and silicates controlled the initial temperature and composit
 ion of the Earth. Current parameterizations of the equilibration efficienc
 y neglect the influence of planetary rotation after impact.\n\nIn a differ
 ent planetary context\, the icy moon Ganymede sustains an intrinsic magnet
 ic field\, likely generated by fluid motions in its iron-rich liquid core.
  Core evolution models suggest solidification proceeds from the outer boun
 dary inward\, producing dense\, pure iron crystals that sink and remelt at
  greater depth. This process\, referred to as “iron snow”\, is thought
  to drive core dynamics that feed the magnetic field. Yet\, it is commonly
  modeled as purely fluid convection\, neglecting the presence and properti
 es of solid particles.
LOCATION:Department of Earth Sciences\, Tilley Lecture Theatre
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