We trace the evolution of a spherically symmetric density perturbation in the MOdified Newtonian Dynamics (MOND) model. The background cosmological model is a \Lambda-dominated, low-\Omega b Friedmann model with no Cold Dark Matter. We include thermal processes and non-equilibrium chemical evolution of the collapsing gas. We find that the first density perturbations which collapse to form luminous objects have mass \sim 105 M\odot . The time of the final collapse of these objects depends mainly on the value of the MOND acceleration a0 and also on the baryon density \Omega b. For the ``standard'' value a0=1.2\times 10-8 cm/s2 the collapse starts at redshift z \sim 160 for \Omega b=0.05 and z \sim 110 for \Omega b=0.02.
PACS numbers: 95.30.Lz, 95.30.Sf, 98.35.Mp, 98.80.Bp
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