Producing baryons from neutralinos in small H2 clumps over cosmological ages
Abstract
Extreme scattering events in quasars suggest the existence of dark H2 clumps of mass 10-3 M and size 10 AU. Such clumps are extremely dense compared to WIMPs clumps of the same mass obtained by N-body simulations. A WIMP clump gravitationally attracted by a central H2 clump would experience a first infall during which its density increases by 106 in 1 Myr. In this poster I begin to explore the phenomenology of mixed clumps made with H2 and WIMPs. Molecular clouds built with clumps are efficient machines to transform smooth distributions of WIMPs into concentrated networks. If WIMPs are neutralinos gravitationally attracted in clumps of such molecular clouds, they may either enrich the baryon sector over cosmological ages, or remain mixed with cold H2 clouds until the clumps evaporate either by collision or by stellar UV heating. A phenomenological model based on an hypothetic dark baryonic component (DBC) that was invoked in the past to explain one of the main drawbacks of CDM profiles, their overly dense cores, is briefly revisited in this context. The DBC is replaced by a mix of H2 and WIMPs, with a small fraction of HI produced by internal H2 collisions, in slightly dispersive clumpy clouds that may migrate from the halo towards inner parts of a galaxy and disk.