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Evolution of magnetic fields in galaxies

MAGNETIC FIELDS ON SCALES FROM KILOPARCECS TO KILOMETERS: PROPERTIES AND ORIGIN Cracow, Poland May 17 – 21, 2010. Evolution of magnetic fields in galaxies. Dmitry Sokoloff Moscow State University Moscow, Russia in collaboration with R.Beck, T.G.Arshakian, M.Krause, D.Moss.

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Evolution of magnetic fields in galaxies

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  1. MAGNETIC FIELDS ON SCALES FROM KILOPARCECS TO KILOMETERS: PROPERTIES AND ORIGIN Cracow, Poland May 17 – 21, 2010 Evolution of magnetic fields in galaxies Dmitry Sokoloff Moscow State University Moscow, Russia in collaboration with R.Beck, T.G.Arshakian, M.Krause, D.Moss

  2. We understand more or less how to fit magnetic fields in contemporary spiral galaxis by conventional dynamo models It requires a detailed knowledge of galactic HD, dynamo governing parameters etc. A detailed analysis of observations for a particular galaxy. A typical example here is M31.

  3. Future observations by SKA Large redshifts z, remote galaxies. Very little is known concerning HD, evolution etc. A reasonable decision would be to postpone with any prediction.... An expected development: no observations in future A demand: give a hint what do you expect for magnetic fields of first galaxies

  4. Seeds in protogalaxies + conventional mean-field dynamo A most straightforward set of parameters -----> time is too short

  5. Seed in protogalaxies + small-scale dynamo + mean-field dynamo It works!!!! A stage of spotty structure. In principle one can observe it.

  6. We can play with parameters. Dwarf galaxies.

  7. Homogeneous relic field+ dynamo: it works unexpectedly bad (recent simulations of D.Moss)

  8. Rotation expels homogeneous field on the remote part of the galaxy(recent simulations of D.Moss)

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