A no-go theorem excludes Gamma in [0,d] for typical non-topological non-relativistic spherically symmetric solitons, with the same exclusion for barotropic fluid compact objects, ruling out natural soliton explanations for observed dark matter halo cores with Gamma ~1.7.
Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions: I. Analytical results
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abstract
We provide an approximate analytical expression of the mass-radius relation of a Newtonian self-gravitating Bose-Einstein condensate (BEC) with short-range interactions described by the Gross-Pitaevskii-Poisson system. These equations model astrophysical objects such as boson stars and, presumably, dark matter galactic halos. Our study connects the non-interacting case studied by Ruffini & Bonazzola (1969) to the Thomas-Fermi limit studied by B\"ohmer & Harko (2007). For repulsive short-range interactions (positive scattering lengths), there exists configurations of arbitrary mass but their radius is always larger than a minimum value. For attractive short-range interactions (negative scattering lengths), equilibrium configurations only exist below a maximum mass. Above that mass, the system is expected to collapse and form a black hole. We also study the radius versus scattering length relation for a given mass. We find that stable configurations only exist above a (negative) minimum scattering length. Our approximate analytical solution, based on a Gaussian ansatz, provides a very good agreement with the exact solution obtained by numerically solving a nonlinear differential equation representing hydrostatic equilibrium. Our treatment is, however, easier to handle and permits to study the stability problem, and derive an analytical expression of the pulsation period, by developing an analogy with a simple mechanical problem.
verdicts
UNVERDICTED 4representative citing papers
Numerical and analytic modeling of boson star-black hole systems in the nonrelativistic limit, with Fisher analysis indicating LISA sensitivity to ultralight dark matter mass and self-coupling via gravitational wave dephasing.
Fisher-matrix forecasts show Cosmic Explorer and Einstein Telescope can probe sub-solar PBHs to z~3 and distinguish PBHs from neutron stars up to z~0.2 via lack of tidal deformability.
Boson stars are particle-like solutions in general relativity that model dark matter, black hole mimickers, and binary systems.
citing papers explorer
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A No-Go Theorem for the Mass-Radius Relation of Solitons
A no-go theorem excludes Gamma in [0,d] for typical non-topological non-relativistic spherically symmetric solitons, with the same exclusion for barotropic fluid compact objects, ruling out natural soliton explanations for observed dark matter halo cores with Gamma ~1.7.
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Boson Stars Hosting Black Holes
Numerical and analytic modeling of boson star-black hole systems in the nonrelativistic limit, with Fisher analysis indicating LISA sensitivity to ultralight dark matter mass and self-coupling via gravitational wave dephasing.
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Primordial black holes versus their impersonators at gravitational wave observatories
Fisher-matrix forecasts show Cosmic Explorer and Einstein Telescope can probe sub-solar PBHs to z~3 and distinguish PBHs from neutron stars up to z~0.2 via lack of tidal deformability.
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Dynamical Boson Stars
Boson stars are particle-like solutions in general relativity that model dark matter, black hole mimickers, and binary systems.