Stability of boson-fermion stars

Henriques, Alfredo B.; Liddle, Andrew R.; Moorhouse, R. G.

doi:10.1016/0370-2693(90)90789-9

Cited by 58 publications

(61 citation statements)

References 9 publications

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“…One can still analyze their stability, among other alternatives, by studying the radial perturbations of these equilibrium configurations and then analyzing the eigenvalues of these modes in the linearized equations as in [15][16][17][18][19], or by evolving dynamically these perturbations by solving the full nonlinear equation of motion [20][21][22][23]. In [24,25] Henriques et al described a method to perform the analysis of stability of the boson-fermion stars by using the binding energy and the number of bosonic and fermionic particles as a function of the two free parameters. In this paper, we propose a similar criterion, and our results are compared with the full numerical solution of the equations of motion.…”

Section: Introductionmentioning

confidence: 99%

Dynamical evolution of fermion-boson stars

et al. 2013

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Compact objects, like neutron stars and white dwarfs, may accrete dark matter, and then be sensitive probes of its presence. These compact stars with a dark matter component can be modeled by a perfect fluid minimally coupled to a complex scalar field (representing a bosonic dark matter component), resulting in objects known as fermion-boson stars. We have performed the dynamical evolution of these stars in order to analyze their stability, and to study their spectrum of normal modes, which may reveal the amount of dark matter in the system. Their stability analysis shows a structure similar to that of an isolated (fermion or boson) star, with equilibrium configurations either laying on the stable or on the unstable branch. The analysis of the spectrum of normal modes indicates the presence of new oscillation modes in the fermionic part of the star, which result from the coupling to the bosonic component through the gravity.

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Section: Introductionmentioning

confidence: 99%

Dynamical evolution of fermion-boson stars

et al. 2013

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“…Finally, we anticipate that the Newtonian approach to the boson star would be valid for a multi-scalar system with many U(1) charges, such as the 'multi-state boson star' [23], and the boson-fermion system [24][25][26][27], in order to extract its inherent characteristics in an efficient manner.…”

Section: Summary and Prospectsmentioning

confidence: 99%

Analytical approximation for Newtonian boson stars in four and five dimensions

Kan

Shiraishi

2016

Phys. Rev. D

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In this paper, we study rotating boson stars in the large coupling limit as well as in the Newtonian limit. We investigate the equilibrium solutions in four and five dimensions by adopting some analytical approximations. We show that the relations among the radius, angular momentum, Newtonian energy, and quadrupole moment (for the four-dimensional solution) of the boson star can be qualitatively realized for the minimal number of boson-star parameters.

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“…We expand the scalar field in terms of creation and annihilation operators in the usual manner [15,16,17], in such a way that ϕ + = ϕ, as is appropriate for a real field:…”

Section: The Modelmentioning

confidence: 99%

“…For a more complete discussion of the issue of stability in boson-fermion stars we refer the reader to [16]. Although we cannot separate the mass of the fermionic component of the star, we introduce in addition, as a useful approximation, but only as an approximation, the following quantity for the fermion core:…”

Section: The Modelmentioning

confidence: 99%

“…Their stability and main properties have been investigated in [16,17,18]. Generalising simple heuristic arguments by Thirring [19], it was then pointed out that many of the general properties could be understood on the basis of an interplay between the Pauli principle and the Heisenberg principle, the first being ultimately responsible for the stability of the fermionic component and the uncertainty principle being responsible for the stability of the bosonic component.…”

Section: Introductionmentioning

confidence: 99%

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