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- W2034383605 abstract "Numerical simulations play an important role in the study of the structure formation of the universe. However, the mass resolution in current simulations is still poor. Due to technical difficulties, it is necessary to use both a greatly reduced number density of particles and a greatly raised unit particle mass. Consequently, the particle masses used in cosmological simulations are about 1070 times larger than the GeV candidates in particle physics. This is a huge physical bias that cannot be neglected when interpreting the results of the simulations. Here we discuss how such a bias affects cold dark matter (CDM) cosmological simulations. We find that the small-scale properties of the CDM particle system are changed in two aspects. (1) An upper limit is imposed on the spatial resolution of the simulation results. (2) Most importantly, an unexpected short mean free path is produced, and the corresponding two-body scattering cross section is close to the value expected in the self-interaction dark matter model. Since the mean free path of real CDM particle systems is much longer than that in the simulations, our results imply that (1) there is probably no cusp problem in real CDM halos and (2) a much longer time is needed to form new virialized halos in real CDM particle systems than in the simulations. The last result can help us understand the substructure problem. Our discussion can also explain why the massive halos in the simulations may have smaller concentration coefficients." @default.
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- W2034383605 date "2004-11-22" @default.
- W2034383605 modified "2023-09-26" @default.
- W2034383605 title "A Physical Bias in Cosmological Simulations" @default.
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- W2034383605 doi "https://doi.org/10.1086/427385" @default.
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