Small Scale Structure Formation in Chameleon Cosmology

Details Small Scale Structure Formation in Chameleon Cosmology Small Scale Structure Formation in Chameleon Cosmology

2005-09-29

arxiv.org/abs/astro-ph/0509878v1

Phys.Lett.B633:441-446,2006

Astronomy and Astrophysics

Astrophysics

13 pages, 4 figures

Scientific paper

10.1016/j.physletb.2005.12.055

Chameleon fields are scalar fields whose mass depends on the ambient matter density. We investigate the effects of these fields on the growth of density perturbations on sub-galactic scales and the formation of the first dark matter halos. Density perturbations on comoving scales $R < 1 {\rm pc}$ go non--linear and collapse to form structure much earlier than in standard $\Lambda$CDM cosmology. The resulting mini-halos are hence more dense and resilient to disruption. We therefore expect (provided that the density perturbations on these scales have not been erased by damping processes) that the dark matter distribution on small scales would be more clumpy in chameleon cosmology than in the $\Lambda$CDM model.

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