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CATEGORIES:Galaxies Discussion Group
SUMMARY:Magnetised clouds in the Galactic corona: Fuel for
  future star formation? - Asger Gronnow (Universit
 y of Sydney)
DTSTART;TZID=Europe/London:20181012T113000
DTEND;TZID=Europe/London:20181012T123000
UID:TALK108805AThttp://talks.cam.ac.uk
URL:http://talks.cam.ac.uk/talk/index/108805
DESCRIPTION:The Galactic halo contains a complex ecosystem of 
 multiphase intermediate-velocity and high-velocity
  gas clouds whose origin has defied clear explanat
 ion. 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 h
 ow the magnetic field in the halo affects these pr
 ocesses using magnetohydrodynamic (MHD) simulation
 s. The magnetic field becomes 'draped' around the 
 clouds as they move through the halo and this fiel
 d suppresses hydrodynamic instabilities at the clo
 ud-halo interface. This has widespread implication
 s for gas accretion. The suppression of instabilit
 ies prolongs the survival of High-Velocity Clouds 
 (HVCs) so that they are more likely to reach the d
 isk. It also suppresses the mixing of cloud-halo m
 aterial in the wakes of clouds ejected by the Gala
 ctic fountain. This leads to less condensation of 
 cold gas that can be accreted through the fountain
  process. In addition\, the draping of the magneti
 c field around clouds means that observational con
 straints on magnetic fields around HVCs can be use
 d to roughly infer their distances. This is useful
  to constrain their masses and thereby how importa
 nt they are as a source of accretion.
LOCATION:Kavli Large Meeting Room\, Kavli Building
CONTACT:Martin Haehnelt
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