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• W3106076548 abstract "A series of high-resolution numerical simulations were performed to study the structure and substructure of Milky Way-sized (MW-sized) and cluster-sized halos in a ΛCDM cosmology with self-interacting (SI) dark matter particles. The cross section per unit of particle mass has the form σDM = σ0(1/v100)α, where σ0 is a constant in units of cm2 g-1 and v100 is the relative velocity in units of 100 km s-1. Different values for σ0 with α = 0 or 1 were used. For small values of σDM = const (≲0.5, α = 0), the core density of the halos at z = 0 is typically higher at a given mass for lower values of σ0 or, at a given σ0, for lower masses. For values of σ0 as high as 3.0, both cluster- and MW-sized halos may undergo the gravothermal catastrophe before z = 0. The core expansion occurs in a stable regime because the heat capacity C is positive in the center. After the maximum expansion, the isothermal core is hotter than the periphery and C < 0. Then the gravothermal catastrophe is triggered. The instability onset can be delayed by both the dynamical heating of the halo by major mergers and the interaction of cool particles with the hot environment of a host halo. When α = 1, the core density of cluster- and MW-sized halos is similar. Using σDM = 0.5-1.0(1/v100), our predictions agree with the central densities and the core scaling laws of halos inferred from the observations of both dwarf and low surface brightness galaxies and clusters of galaxies. Regarding the cumulative vmax function of subhalos within MW-sized halos, when (σ0, α) = (0.1, 0.0), (0.5, 0.0), or (0.5, 1.0) it agrees roughly with observations (luminous satellites) for vmax ≳ 30 km s-1, while at vmax = 20 km s-1 the functions are already a factor of 5-8 higher, similar to the CDM predictions. For (σ0, α) = (1.0, 1.0), this function lies above the corresponding CDM function. The structure and number of subhalos are affected by the scattering properties of the host halo rather than by those of the subhalos. The halos with SI have more specific angular momentum at a given mass shell and are rounder than their CDM counterparts. However, the angular momentum excess with regard to CDM is small. We conclude that the introduction of SI particles with σDM ∝ 1/v100 may remedy the cuspy core problem of the CDM cosmogony, at the same time keeping a subhalo population similar to that of the CDM halos." @default.
• W3106076548 created "2020-11-23" @default.
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• W3106076548 date "2002-12-20" @default.
• W3106076548 modified "2023-10-16" @default.
• W3106076548 title "Structure and Subhalo Population of Halos in a Self‐interacting Dark Matter Cosmology" @default.
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• W3106076548 doi "https://doi.org/10.1086/344259" @default.
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