First simulations of axion minicluster halos. (arXiv:1911.09417v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Eggemeier_B/0/1/0/all/0/1">Benedikt Eggemeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Redondo_J/0/1/0/all/0/1">Javier Redondo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolag_K/0/1/0/all/0/1">Klaus Dolag</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemeyer_J/0/1/0/all/0/1">Jens C. Niemeyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaquero_A/0/1/0/all/0/1">Alejandro Vaquero</a>
We study the gravitational collapse of axion dark matter fluctuations in the
post-inflationary scenario, so-called axion miniclusters, with N-body
simulations. Largely confirming theoretical expectations, overdensities begin
to collapse in the radiation-dominated epoch and form an early distribution of
miniclusters with masses up to $10^{-12},M_odot$. After matter-radiation
equality, ongoing mergers give rise to a steep power-law distribution of
minicluster halo masses. The density profiles of well-resolved halos are
NFW-like to good approximation. The fraction of axion DM in these bound
structures is $sim 0.75$ at redshift $z=100$.
We study the gravitational collapse of axion dark matter fluctuations in the
post-inflationary scenario, so-called axion miniclusters, with N-body
simulations. Largely confirming theoretical expectations, overdensities begin
to collapse in the radiation-dominated epoch and form an early distribution of
miniclusters with masses up to $10^{-12},M_odot$. After matter-radiation
equality, ongoing mergers give rise to a steep power-law distribution of
minicluster halo masses. The density profiles of well-resolved halos are
NFW-like to good approximation. The fraction of axion DM in these bound
structures is $sim 0.75$ at redshift $z=100$.
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