Speaker
Description
As a component of the cosmic web, filaments are important for us to understand the formation of the large scale structure.
In this work, we study the influence of angular momentum, filament growth history, and cosmic expansion on filament density profiles.
We present two models characterizing dark matter filament growth implementing the stretch of filaments, the power law growth model (the PL model) and the M18 model, in which the growth of filaments is derived from the growth history of halos.
For the PL model, the density profiles follow $\rho\propto r^{-1}$ in the inner region of the filaments for a purely infall case, which is consistent with the results by Fillmore$\&$Goldreich.
We found that in the case of larger tangential velocity, higher growth rate, and stronger expansion, the filament density profiles are more cored.
We also propose a new model for the splashback radius of filaments.
For the M18 model, we found consistence of density profiles with simulation results.
Although future work is needed to calibrate the growth history of filaments, our work could provide a framework for analyzing the formation of filaments as well as the environment around filaments.
