Stability of BEC galactic dark matter halos

TL;DR

This paper demonstrates that spherically symmetric BEC dark matter halos with a specific density profile are dynamically unstable, losing mass rapidly and thus unlikely to be viable models for galactic halos.

Contribution

The study provides a numerical analysis showing the instability of BEC dark matter halos with a sine-based density profile, challenging their viability as galactic models.

Findings

Halos lose about half their mass in tens of millions of years.

The instability appears to be a general feature of these models.

Several drawbacks restrict the model's physical viability.

Abstract

In this paper we show that spherically symmetric BEC dark matter halos, with the $\sin r/r$ density profile, that accurately fit galactic rotation curves and represent a potential solution to the cusp-core problem are unstable. We do this by introducing back the density profiles into the fully time-dependent Gross-Pitaevskii-Poisson system of equations. Using numerical methods to track the evolution of the system, we found that these galactic halos lose mass at an approximate rate of half of its mass in a time scale of dozens of Myr. We consider this time scale is enough as to consider these halos are unstable and unlikely to be formed. We provide some arguments to show that this behavior is general and discuss some other drawbacks of the model that restrict its viability.