Axion miniclusters and Bose stars.

@article{Kolb1993AxionMA,
  title={Axion miniclusters and Bose stars.},
  author={Kolb and Tkachev},
  journal={Physical review letters},
  year={1993},
  volume={71 19},
  pages={
          3051-3054
        }
}
  • Kolb, Tkachev
  • Published 29 March 1993
  • Physics, Materials Science
  • Physical review letters
Evolution of inhomogeneities in the axion field around the QCD epoch is studied numerically, including for the first time important nonlinear effects. It is found that perturbations on scales corresponding to causally disconnected regions at T\ensuremath{\sim}1 GeV can lead to very dense axion clumps, with present density ${\mathrm{\ensuremath{\rho}}}_{\mathit{a}}$\ensuremath{\gtrsim}${10}^{\mathrm{\ensuremath{-}}8}$ g ${\mathrm{cm}}^{\mathrm{\ensuremath{-}}3}$. This is high enough for the… 

Astrophysical Effects of Scalar Dark Matter Miniclusters

We model the formation, evolution and astrophysical effects of dark compact Scalar Miniclusters (``ScaMs''). These objects arise when a scalar field, with an axion-like or Higgs-like potential,

ON THE EXISTENCE OF THE SUPERSTRING AXION MINI-STAR

It is shown that the lasing mechanism of axion solitonic stars found by Tkachev is suppressed above a critical value of the QCD decay constant fa ≈ 1015GeV. This means, in particular, that the

Axion star nucleation in dark minihalos around primordial black holes

We consider a general class of axion models, including the QCD and string axion, in which the PQ symmetry is broken before or during inflation. Assuming the axion is the dominant component of the

The Lifetime of Axion Stars

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

Do dark matter axions form a condensate with long-range correlation?

TLDR
The authors investigate the formation of Bose-Einstein condensates from axion dark matter, and it is shown that a homogeneous condensate with long range correlations is unstable when interactions like gravity are taken into account.

Scalar field “mini-MACHOs”: A new explanation for galactic dark matter

We examine the possibility that galactic halos are collisionless ensembles of scalar field ``massive compact halo objects'' (MACHOs). Using mass constraints from MACHO microlensing and from

Moduli stars

A bstractWe explore the possibility that (Bose-Einstein) condensation of scalar fields from string compactifications can lead to long-lived compact objects. Depending on the type of scalar fields we

Dense Axion Stars.

TLDR
A new branch of dense axion stars is found in which gravity is balanced by the mean-field pressure of the axion Bose-Einstein condensate, and this branch could produce a bosenova, leaving a dense axions star as the remnant.

Gravitational waves from binary axionic black holes

In a recent paper we have shown that a minimally coupled, self-interacting scalar field of mass m can form black holes of mass $$M=\sqrt{3}/(4m)$$M=3/(4m) (in Planck units). If dark matter is

Early seeds of axion miniclusters

We study the small scale structure of axion dark matter in the post-inflationary scenario, which predicts the formation of low-mass, high density clumps of gravitationally bound axions called axion
...

References

SHOWING 1-9 OF 9 REFERENCES

The early Universe

In the past few years one of the most exciting areas of research in physics has been the interdisciplinary field of cosmology and particle physics. The NSF's Institute for Theoretical Physics in

Phys. Rev. Phys. Lett. B140

  • Phys. Rev. Phys. Lett. B140
  • 1969

I. I. Tkachev, Sov. Astron. Lett

  • I. I. Tkachev, Sov. Astron. Lett
  • 1986

Rev. Mod. Phys

  • Rev. Mod. Phys
  • 1981

Phys. Rev. D

  • Phys. Rev. D
  • 1986

Phys. Rep. C197 Phys. Rep. C198

  • Phys. Rep. C197 Phys. Rep. C198
  • 1990

This does not necessarily require the reheating temperature after inflation to be higher than f a , since inflation itself can produce strong fluctuations in the axion field as discussed in

  • Phys. Lett
  • 1990

Phys. Rev. Lett

  • Phys. Rev. Lett
  • 1983

We will discuss in a future paper the possibility that collapsing domain walls leave behind very dense clumps of non-relativistic axions