Abstract
We study self-gravitating bosonic systems, candidates for dark-matter halos, by carrying out a suite of direct numerical simulations (DNSs) designed to investigate the formation of finitetemperature, compact objects in the three-dimensional (3D) Fourier-truncated Gross-Pitaevskii-Poisson equation (GPPE). This truncation allows us to explore the collapse and fluctuations of compact objects, which form at both zero temperature and finite temperature. We show that the statistically steady state of the GPPE, in the large-time limit and for the system sizes we study, can also be obtained efficiently by tuning the temperature in an auxiliary stochastic Ginzburg-Landau-Poisson equation (SGLPE). We show that, over a wide range of model parameters, this system undergoes a thermally driven first-order transition from a collapsed, compact, Bose-Einstein condensate (BEC) to a tenuous Bose gas without condensation. By a suitable choice of initial conditions in the GPPE, we also obtain a binary condensate that comprises a pair of collapsed objects rotating around their center of mass.
Highlights
Gravitational effects are important on stellar scales; it might be possible to mimic such effects in laboratory Bose-Einstein condensates (BEC) [1] and emulate gravitationally bound, condensed assemblies of bosons, which are candidates for dark-matter halos [2,3,4,5]
We study self-gravitating bosonic systems, candidates for dark-matter halos, by carrying out a suite of direct numerical simulations designed to investigate the formation of finite-temperature, compact objects in the three-dimensional (3D) Fourier-truncated Gross-Pitaevskii-Poisson equation (GPPE)
By a suitable choice of initial conditions in the GPPE, we obtain a binary condensate that comprises a pair of collapsed objects rotating around their center of mass
Summary
The subtraction of the mean density |ψ|2 can be justified either by taking into account the cosmological expansion [19,20] or by defining a Newtonian cosmological constant [21]. By linearizing Eq (1) around the constant |ψ|2 = n0, we obtain the dispersion relation ω(k) =. −Gn0/m + k2gn0/m + k4(h/2m), which has been studied in detail in Ref. This dispersion relation displays a low-k Jeans instability for wave numbers k < kJ =
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