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SUMMARY:Magnetic field in early galaxies
DTSTART;VALUE=DATE-TIME:20090422T100000Z
DTEND;VALUE=DATE-TIME:20090422T110000Z
DTSTAMP;VALUE=DATE-TIME:20261109T154344Z
UID:indico-event-1689@indico.ific.uv.es
DESCRIPTION:In the context of models of galaxy formation and evolution\, t
 he cosmological evolution of large- and small-scale magnetic fields inside
  galaxies is discussed. We use the dynamo theory to derive the timescales 
 of amplification and ordering of magnetic fields in disk and puffy galaxie
 s. Turbulence in protogalactic halos generated by thermal virialization ca
 n drive an efficient turbulent dynamo. The turbulent (small-scale) dynamo 
 was able to amplify a weak seed magnetic field in halos of protogalaxies t
 o a few μG strength within a few 108 yr. This turbulent field served as a
  seed to the mean-field (large-scale) dynamo. Galaxies similar to the Milk
 y Way formed their disks at z≈10 and regular fields of μG strength and 
 a few kpc coherence length were generated within 2 Gyr (at z≈3)\, but fi
 eld-ordering on the coherence scale of the galaxy size required an additio
 nal 6 Gyr (at z≈0.5). Giant galaxies formed their disks at z≈10\, allo
 wing more efficient dynamo generation of strong regular fields (with kpc c
 oherence length) already at z≈4. However\, the age of the Universe is sh
 ort for fully coherent fields in giant galaxies larger than 15 kpc to have
  been achieved. Dwarf galaxies should have hosted fully coherent fields at
  z≈1. After a major merger\, the strength of the turbulent field is enha
 nced by a factor of a few. This evolutionary scenario can be tested by mea
 surements of polarized synchrotron emission and Faraday rotation with the 
 planned Square Kilometre Array (SKA).\n\nhttps://indico.ific.uv.es/event/1
 689/
LOCATION:Edf. Institutos de Investigación Sala Seminarios IFIC
URL:https://indico.ific.uv.es/event/1689/
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