Random fluctuation walk in the boson star formation process

TL;DR

This paper models the formation of scalar boson stars using a random walk approach, analyzing the dynamics of dark matter lumps and phase cross-over with power-law growth and critical temperature bounds.

Contribution

It introduces a novel random fluctuation walk framework to study boson star formation, incorporating self-similar dark matter lumps and phase transition dynamics.

Findings

Derived the probability functional for DM and condensate phases.

Presented power-law growth models for boson star formation.

Calculated bounds on critical temperature for phase cross-over.

Abstract

We construct the mechanism of formation of the scalar boson star (BS) having a hierarchy of self-similar "lumps" of dark matter (DM) built into the probability distribution function of allowed steps. It can ensure to study the dynamics of the BS formation through the "cross-over" between the free scalar DM and the compact condensate (CC) phase in one-dimensional model of the random fluctuation walk. The main inputs are the random fluctuating weight $\lambda < 1$, the fundamental fluctuating length $\xi (\lambda)$ and the parameter $a >1$ of the spatial separation between the DM "lumps" inside the BS. The solution to the functional equation for the characteristic probability to find the free scalar DM and the CC phase is obtained. The time evolution of the probability to form the DM "lump" (growth of the BS) is presented with the power-law cascades expression depending on $\lambda$ and $a$. The special cases for $\lambda$ in terms of the energy densities of the BS ($\rho_\star$) and the DM ($\rho_\odot$), as well as the Bose-Einstein correlation function for two scalar DM particles, are considered. The lower bounds on the critical temperature at the "cross-over" depending on $\rho_\odot$, $\rho_\star$, the average multiplicities of the scalar DM particles and the parameters related to the chaotically behaviour of the particles are obtained.