Chains of rotating boson stars

Gervalle, Romain

doi:10.1103/physrevd.105.124052

Cited by 9 publications

(3 citation statements)

References 45 publications

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“…Typically [18][19][20][21][23][24][25][26][27][28][29][30][31][32]35], the profile for the scalar field of a rotating Q-ball or boson star is assumed to take the form…”

Section: Rotating Q-ballsmentioning

confidence: 99%

“…This is a normal assumption for collapse to black holes or disks, for which any angular momentum is allowed. However, for rotating Q-balls [18][19][20][21][22][23] (and the closely related boson stars [24][25][26][27][28][29][30][31][32][33][34][35][36]) the dominant paradigm is that the angular momentum must be an integer multiple of the charge Q. If this is the case, then the formation of large Q-balls would be drastically different from the usual collapse, since angular momentum would need to be shed in a very precise manner.…”

Section: Introductionmentioning

confidence: 99%

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Slowly rotating Q-balls

Almumin,

Heeck,

Rajaraman

et al. 2024

Eur. Phys. J. C

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Q-balls are non-topological solitons arising in scalar field theories. Solutions for rotating Q-balls (and the related boson stars) have been shown to exist when the angular momentum is equal to an integer multiple of the Q-ball charge Q. Here we consider the possibility of classically long-lived metastable rotating Q-balls with small angular momentum, even for large charge, for all scalar theories that support non-rotating Q-balls. This is relevant for rotating extensions of Q-balls and related solitons such as boson stars as it impacts their cosmological phenomenology.arXiv:2302.11589

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“…Typically [18][19][20][21][23][24][25][26][27][28][29][30][31][32]35], the profile for the scalar field of a rotating Q-ball or boson star is assumed to take the form…”

Section: Rotating Q-ballsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Slowly rotating Q-balls

Almumin,

Heeck,

Rajaraman

et al. 2024

Eur. Phys. J. C

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show abstract

“…[2,. In some cases, multi-centre stars, which can be interpreted as several boson stars in equilibrium have also been reported [49][50][51][52][53][54]. A key aspect of boson stars is that they are dynamically robust, for some models and in parts of the parameter space [55][56][57][58][59][60][61][62][63][64][65][66], allowing dynamical strong gravity studies, such as collisions and mergers of individual stars, to test their stability and obtain to gravitational wave templates -see e.g.…”

Section: Introductionmentioning

confidence: 99%

Proca-Higgs balls and stars in a UV completion for Proca self-interactions

Herdeiro

Radu

Filho

2023

J. Cosmol. Astropart. Phys.

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We consider a Proca-Higgs model wherein a complex vector field gains mass via spontaneous symmetry breaking, by coupling to a real scalar field with a Higgs-type potential. This vector version of the scalar Friedberg-Lee-Sirlin model, can be considered as a UV completion of a complex Proca model with self-interactions. We study the flat spacetime and self-gravitating solitons of the model, that we dub Proca-Higgs balls and stars respectively, exploring the domain of solutions and describing some of their mathematical and physical properties. The stars reduce to the well-known (mini-)Proca stars in some limits. The full model evades the hyperbolicity problems of the self-interacting Proca models, offering novel possibilities for dynamical studies beyond mini-Proca stars.

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Chains of mini-boson stars

Sun,

Zhao,

Wang

2023

J. High Energ. Phys.

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In this paper, we re-investigate the static, soliton-like solutions in the model of the Einstein gravity coupled to a free and complex scalar field, which have been known as mini-boson stars. With the numerical methods, we have discovered a new family of solutions in addition to the typical single mini-boson star solution. These solutions can be interpreted as chains of boson stars, consisting of multiple boson stars along the symmetry axis. We demonstrate the configuration of two types of chains, one with an even number of constituents and the other with an odd number of constituents. Furthermore, we also study the effect of the frequency of the complex scalar field on the ADM mass M and the U(1) scalar charge Q. It is noteworthy that the existence of chains of boson stars does not require the introduction of a complex scalar field with self-interacting potential.

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Chains of rotating boson stars

Cited by 9 publications

References 45 publications

Slowly rotating Q-balls

Slowly rotating Q-balls

Proca-Higgs balls and stars in a UV completion for Proca self-interactions

Chains of mini-boson stars

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