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SUMMARY:Magnetised clouds in the Galactic corona: Fuel for future star for
 mation? - Asger Gronnow (University of Sydney)
DTSTART:20181012T103000Z
DTEND:20181012T113000Z
UID:TALK108805@talks.cam.ac.uk
CONTACT:Martin Haehnelt
DESCRIPTION:The Galactic halo contains a complex ecosystem of multiphase i
 ntermediate-velocity and high-velocity gas clouds whose origin has defied 
 clear explanation. They are generally believed to be involved in a Galaxy-
 wide recycling process\, either through an accretion flow or a large-scale
  fountain flow\, or both. In this talk I will present my work on how the m
 agnetic field in the halo affects these processes using magnetohydrodynami
 c (MHD) simulations. The magnetic field becomes 'draped' around the clouds
  as they move through the halo and this field suppresses hydrodynamic inst
 abilities at the cloud-halo interface. This has widespread implications fo
 r gas accretion. The suppression of instabilities prolongs the survival of
  High-Velocity Clouds (HVCs) so that they are more likely to reach the dis
 k. It also suppresses the mixing of cloud-halo material in the wakes of cl
 ouds ejected by the Galactic fountain. This leads to less condensation of 
 cold gas that can be accreted through the fountain process. In addition\, 
 the draping of the magnetic field around clouds means that observational c
 onstraints on magnetic fields around HVCs can be used to roughly infer the
 ir distances. This is useful to constrain their masses and thereby how imp
 ortant they are as a source of accretion.
LOCATION:Kavli Large Meeting Room\, Kavli Building
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