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Numerical evolutions of spherical Proca stars
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abstract
Vector boson stars, or $\textit{Proca stars}$, have been recently obtained as fully non-linear numerical solutions of the Einstein-(complex)-Proca system. These are self-gravitating, everywhere non-singular, horizonless Bose-Einstein condensates of a massive vector field, which resemble in many ways, but not all, their scalar cousins, the well-known (scalar) $\textit{boson stars}$. In this paper we report fully-non linear numerical evolutions of Proca stars, focusing on the spherically symmetric case, with the goal of assessing their stability and the end-point of the evolution of the unstable stars. Previous results from linear perturbation theory indicate the separation between stable and unstable configurations occurs at the solution with maximal ADM mass. Our simulations confirm this result. Evolving numerically unstable solutions, we find, depending on the sign of the binding energy of the solution and on the perturbation, three different outcomes: $(i)$ migration to the stable branch, $(ii)$ total dispersion of the scalar field, or $(iii)$ collapse to a Schwarzschild black hole. In the latter case, a long lived Proca field remnant -- a $\textit{Proca wig}$ -- composed by quasi-bound states, may be seen outside the horizon after its formation, with a life-time that scales inversely with the Proca mass. We comment on the similarities/differences with the scalar case as well as with neutron stars.
Forward citations
Cited by 8 Pith papers
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Core-Halo Mass Relation in Cosmological Vector Dark Matter
Confirmed Proca-star cores in vector dark matter follow M_star ≈ 2.65 M_halo^0.64, with only about 10% of halos hosting a detectable core.
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Stable dipolar boson stars and flat-space Q-ball chains are constructed in the Friedberg-Lee-Sirlin model, and chains beyond the dipole are found unstable in tested cases.
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Extreme mass-ratio inspirals into Newtonian Proca stars
For Newtonian Proca stars, a perturbing object on a circular orbit loses nearly the same energy in the vector ground state as in the scalar boson-star ground state (within ~20%), while the spherical excited Proca stat...
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Quasi-bound states and late-time evolution of a massive fermion around a Reissner-Nordstr\"{o}m black hole
Matrix matching yields improved quasi-bound spectra (fine structure + decay widths) for a massive Dirac field on RN, and branch-cut analysis plus simulations reveal an intermediate oscillatory power law followed by a ...
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Bifurcations in Bosonic Stars: chains and rings from spherical solutions
Zero-modes of spherical bosonic stars under axisymmetric perturbations explain the bifurcations into chain, ring, and gyroscope-like bosonic star families.
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Nonrelativistic Proca stars: Spherical stationary and multi-frequency states
Nonrelativistic Proca stars have a ground state with constant polarization (linear or circular depending on the sign of the spin-spin coupling), and a symmetry-enhanced sector with λs=0 contains a continuum of multi-f...
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Proca stars in excited states
Excited Proca stars are always unstable: under perturbations they collapse, disperse, or migrate to the ground state, with migration possible only for a narrow set of negative-binding-energy configurations.
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The continuum spectrum of nonrelativistic multi-frequency Proca stars
At fixed particle number, spherical multi-frequency Proca stars form continuous 1- and 2-parameter families interpolating between discrete stationary states, and a subset with a nodeless component is linearly stable.
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