Simulations including gas
Simulations Including Gas

Simulations of InterGalacticMedium/
Simulations of Galaxy Formation/
SPH/N-body Simulations of Clusters

Simulations of InterGalacticMedium

Tom Theuns and his collaborators are studying the evolution of the Ly_alpha forests at high redshifts.

Pic.1 Gas density distribution in a volume of size 11x11x1.35 (h-1Mpc)3. High density regions are yellow, low density regions are black. The mass resolution is 1.5 x 106 Msun. The gas has a characteristic filamentary appearance, with high density knots corresponding to forming galaxies at the intersection of two or more filaments.
 PS format(150KB)/ GIF format(120KB)
Credit: Tom Theuns, ref.1

Pic.2 Same as Pic.1, z=5.0.
PS format(180KB)/ GIF format(140KB)
Credit: Tom Theuns, ref.1

Reference
  1. P3M-SPH simulations of the Ly-alpha forest
    T.Theuns, A.Leonard, J.Schaye, G.Efstathiou, F.Pearce, and P.Thomas
    1998,MNRAS,301,478





Hydrodynamic simulation with radiative cooling

Yoshida et al. (2002, see the reference below) used two techniques for following gas cooling in simulations of galaxy formation, and compared the results such as `galaxy' (cold dense gas) masses and their positions.


Pic.1 Projected gas distribution in a box of 15 h-1Mpc.

PS format(150KB)/ GIF format(120KB)
Credit: See ref.2

Pic.2 The distribution of the `galaxies' in the hydrodynamic and semianalytic simulations. The blue-white color scale shows the underlying matter distribution.

SPH simulation (left) and the semi-analytic model (right)

Credit: See ref.2

Reference
  1. Gas cooling in simulations of the formation of the galaxy population
    N. Yoshida, F. Stoehr, V. Springel, and S.D.M. White
    2002, astro-ph/0202341





SPH/N-body Simulations of Clusters

Formation of a cluster size dark halo by collisional and collisionless dark matter

Pic.1 Projected mass distributions in a cube box 15 Mpc/h per oneside (left column) and in the central regions of 2 Mpc/h per one side (enlarged, right column). The picture clearly shows the difference (as well as similarlities in the outer region of the halo) in mass distribution, morphorlogy of the central part, and abundance of subclumps.

Reference
  1. Collisional dark matter and the structure of dark halos
    N.Yoshida, V.Springel, S.D.M.White, G.Tormen
    2000, ApJ, 535, L103 (preprint astro-ph/0002362)

  2. Weakly self-interacting dark matter and the structure of dark halos
    N.Yoshida, V.Springel, S.D.M.White, G.Tormen
    2000, ApJ, 544, L87 (preprint astro-ph/0006134)
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Last modified: Thu Jan 13 13:30:54 MET 2000 by Virgo Administrator