Supernova driven turbulence in the interstellar medium

See below: movies of supernova (SN) driven turbulence in the interstellar medium (ISM). The movie first from the left (in blue) depicts the density of the ISM in which SN remnants appear as dark hollows, where the explosion has forced out the gas leaving a very diffuse remnant interior. The next movie (in red) depicts the temperature. In this case the SN remants appear as light flashes where the explosions heat the ISM to in excess of 10 Million degrees Kelvin. Each face shows a 2D slice through the centre of the box. The midplane of the galaxy is in the centre and our domain extend 1 kiloparsec (kpc) either side of the mid plane and covers an area 1 square kpc representing the radial and azimuthal directions relative to the galactic centre. We model conditions typical of the solar neighbourhood. (1 kpc = 30.86 thousand million million km)

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The latter two movies depict the magnetic field and show the dynamo action of the ISM from a small seed field. The movie on the left shows the magnetic energy distribution and the movie next to it the azimuthal component of the magnetic field. A small seed field of 0.001 micro Gauss is amplified by the turbulence and differential rotation of the galaxy to about 2 micro Gauss.
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Images above: a snap shot of the ISM from a current simulation still transient from the initial hydrostatic state. Shows x-planes through the cube of density, temperature and (below) vertical velocity. A powerful jet has erupted at 1kpc<z<1.5kpc y=-0.5kpc out of a super bubble of SN remnants. Images below: horizontal averages of the evolution of the current ISM model. The first shock waves have now reached the upper boundary, but turbulence is not yet established

Supernova snowplough resolution test

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