Axially symmetric Proca-Higgs boson stars

Dzhunushaliev, Vladimir; Folomeev, Vladimir

doi:10.1103/physrevd.104.104024

Cited by 12 publications

(3 citation statements)

References 45 publications

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“…Next, taking into account the condition for the four-velocity U µ U µ = 1 and making use of the metric (5) and the expression ( 6), the velocity u can be expressed in terms of the metric functions f, l, and ω as follows [written already in terms of the dimensionless variables (7)]:…”

Section: General Equationsmentioning

confidence: 99%

“…The field equations coming from the Einstein equations ( 4) can be represented in the following form [written in terms of the dimensionless variables (7)]:…”

Section: General Equationsmentioning

confidence: 99%

“…Apart from boson stars, a consideration of configurations consisting of fields with nonzero spins is also possible. Such hypothetical systems may be supported by massive vector (spin-1) fields (Proca stars [4][5][6][7]) and massless vector fields (Yang-Mills systems [8,9]). In the case of fractional-spin fields it is also possible to obtain various spherically symmetric systems consisting of gravitating linear [5,10,11] and nonlinear spin-1/2 fields [12][13][14].…”

Section: Introductionmentioning

confidence: 99%

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Rapidly rotating Dirac stars

Dzhunushaliev,

Folomeev,

Burtebayev

2022

Preprint

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Within general relativity, we construct sequences of rapidly rotating Dirac stars consisting of a spinor fluid described by an effective equation of state. We find the physically relevant domain of stable configurations and calculate their principal characteristics which are completely determined by the central density of the spinor fluid, the mass of the nonlinear spinor field, and the velocity of rotation. It is demonstrated that for a certain choice of the spinor field mass the main physical characteristics of the Dirac stars are close to those that are typical of rotating neutron stars.

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Section: General Equationsmentioning

confidence: 99%

“…The field equations coming from the Einstein equations ( 4) can be represented in the following form [written in terms of the dimensionless variables (7)]:…”

Section: General Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Rapidly rotating Dirac stars

Dzhunushaliev,

Folomeev,

Burtebayev

2022

Preprint

Self Cite

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Spinning Proca-Higgs balls, stars and hairy black holes

Herdeiro,

Radu,

dos Santos Costa Filho

2024

J. Cosmol. Astropart. Phys.

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Recently, spherical and static flat space solitons (balls) and self-gravitating, everywhere regular, asymptotically flat solitons (stars) were constructed in an Einstein-Proca-Higgs model [1], where a complex vector field gains mass by coupling to a real scalar field with a Higgs-type potential. The Proca-Higgs model serves as a UV completion of a complex Proca model with self-interactions. Here, we construct and examine the mathematical and physical properties of rotating configurations. In particular, rotation allows horizon-bearing solutions, including stationary clouds surrounding Kerr black holes and their non-linear continuation into black holes with Proca-Higgs hair.

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Axially symmetric particlelike solutions with the flux of a magnetic field in the non-Abelian Proca-Higgs theory

Dzhunushaliev

Folomeev

2021

Phys. Rev. D

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Axially symmetric Proca-Higgs boson stars

Cited by 12 publications

References 45 publications

Rapidly rotating Dirac stars

Rapidly rotating Dirac stars

Spinning Proca-Higgs balls, stars and hairy black holes

Axially symmetric particlelike solutions with the flux of a magnetic field in the non-Abelian Proca-Higgs theory

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