Halo formation in self-interacting dark matter models
امید سمیعی
Omid Sameie
Department of Astronomy, University of Texas Austin
**لطفا به ساعت نامتعارف سمینار توجه فرمایید**
Abstract: Strong dark matter interactions are proposed to alleviate the tension between observations and theoretical predictions in CDM. Among different interaction channels, self-interacting dark matter (SIDM) models have received considerable attention. However, most of the models and simulations have so far neglected the contribution of the baryons. First, I will present a combination of results from idealized SIDM simulations that explore the effect of a baryonic disk/bulge on the shape and density profile of dark matter halos. We find that the inclusion of baryons in these models help to alleviate two of the longstanding issues within CDM: i) the diversity of rotation curves on the scale of dwarf galaxies and ii) the high sphericity measured for the dark matter halo of our own Milky Way. The observations of Milky Way satellite galaxies have also revealed a large spread in their central dark matter densities. In the second part of my talk, I discuss how dark matter self-interactions plus environmental effects such as tidal stripping can reproduce the observed diverse central densities in the Milky Way dwarf spheroidal galaxies. In the third part of my talk I will discuss an analytical model to study the effects of dark matter-dark radiation interactions on the abundance of faint galaxies at high redshifts.
یکشنبه 14 اردیبهشت 1399، ساعت 18:00
Sunday 3 May, 2020 – 18:00 Tehran Time
اتاق سمینار مجازی –Virtual Seminar Room
https://vclass.ecourse.sharif.edu/ch/cosmology
گزینه ورود به صورت مهمان – Enter as a Guest