The Lifetime of Axion Stars

TL;DR

This paper analyzes the decay mechanisms and stability conditions of axion stars, showing that weakly bound axion stars can have long lifetimes due to suppressed decay rates, and maps their stable parameter space.

Contribution

It provides a detailed calculation of axion star decay rates, demonstrating how binding energy affects their stability and survival over cosmological timescales.

Findings

Weakly bound axion stars have exponentially suppressed decay rates.

Stable axion star regions are mapped based on axion and star masses.

Strongly bound axion stars decay rapidly due to high momentum transfer.

Abstract

We investigate the decay of condensates of scalars in a field theory defined by $V({\cal A})=m{}^2\,f{}^2\,[1-\cos({\cal A}\,/\,f)]$, where $m$ and $f$ are the mass and decay constant of the scalar field. An example of such a theory is that of the axion, in which case the condensates are called axion stars. The axion field, $\cal A$, is self adjoint. As a result the axion number is not an absolutely conserved quantity. Therefore, axion stars are not stable and have finite lifetimes. Bound axions, localized on the volume of the star, have a coordinate uncertainty $\Delta x \sim R \sim 1/(m_a \Delta)$, where $R$ is the radius of the star and $\Delta = \sqrt{1-E_0{}^2\,/\,m_a^2}$. Here $m_a$ and $E_0$ are the mass, and the ground state energy of the bound axion. Then the momentum distribution of axions has a width of $\Delta p\sim m_a\,\Delta$. At strong binding, $\Delta={\cal O}(1)$, bound axions can easily transfer a sufficient amount of momentum to create and emit a free axion, leading to fast decay of the star with a transition rate $\Gamma \sim m_a$. However, when $\Delta\ll 1$, the momentum distribution is more restricted, and as shown in this paper, the transition rate for creating a free axion decreases as $\exp (-p \, \Delta x) \sim \exp (-\Delta^{-1})$. Then sufficiently large, weakly bound axion stars, produced after the big bang, survive until the present time. We plot the region of their stability, limited by decay through axion loss and by gravitational instability, as a function of the mass of the axion and the mass of the star.