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 1993
  • Physics, Medicine
  • 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… Expand

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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 inExpand
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. Rev. D
  • 1990
I. I. Tkachev, Sov. Astron. Lett
  • I. I. Tkachev, Sov. Astron. Lett
  • 1986
Phys. Rev. D
  • Phys. Rev. D
  • 1986
Phys. Rev. Lett
  • Phys. Rev. Lett
  • 1983
Rev. Mod. Phys
  • Rev. Mod. Phys
  • 1981
Phys. Rev. Phys. Lett. B140
  • Phys. Rev. Phys. Lett. B140
  • 1969
We will discuss in a future paper the possibility that collapsing domain walls leave behind very dense clumps of non-relativistic axions
  • We will discuss in a future paper the possibility that collapsing domain walls leave behind very dense clumps of non-relativistic axions