Self-gravitating system made of axions

Barranco, J.; Bernal, Argelia

doi:10.1103/physrevd.83.043525

Cited by 121 publications

(133 citation statements)

References 44 publications

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“…The striking feature of the plot is the maximum of the mass as a function of parameter λ = f a / (M P ∆). Maxima of M , as a function of the central value of the axion wave function have already been found in previous work [3,[6][7][8][9][10][11][12], but the maximum in figure 2 has a physical significance due to the following considerations. 2 Note that the number of axions in the condensate is approximately equal to Table 1.…”

Section: Analytic Approximations To the Physical Parameters Of Axion mentioning

confidence: 81%

“…More recently, the authors of [11,12] used a similar procedure to describe the condensation of interacting hermitian Bose fields. We revisit this analysis by evaluating the expectation value of the axion potential in the N particle condensed state and simplifying the equations of motion using the expansion method described in the previous section.…”

Section: Axion Field Dynamics In the Condensed Statementioning

confidence: 99%

“…In a recent set of publications, [11][12][13][14] analyzed the self-gravitating field theoretical system consisting of a real scalar field with an interaction potential of the form f a 2 m a 2 (1 − cos( φ fa )). They followed the method pioneered by Ruffini and Bonazzola.…”

Section: Jhep03(2015)080mentioning

confidence: 99%

“…R 99 continues to increase throughout the range of λ considered. The axion stars investigated in [11,12] correspond to the extremely small values of λ ∼ 10 −6 − 10 −5 . Using fit (3.7), we obtain from (3.5) at λ 1…”

Section: Analytic Approximations To the Physical Parameters Of Axion mentioning

confidence: 99%

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Axion stars in the infrared limit

Eby

Surányi

Vaz

et al. 2015

J. High Energ. Phys.

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Following Ruffini and Bonazzola, we use a quantized boson field to describe condensates of axions forming compact objects. Without substantial modifications, the method can only be applied to axions with decay constant, f a , satisfying δ = (f a / M P ) 2 1, where M P is the Planck mass. Similarly, the applicability of the Ruffini-Bonazzola method to axion stars also requires that the relative binding energy of axions satisfies1, where E a and m a are the energy and mass of the axion. The simultaneous expansion of the equations of motion in δ and ∆ leads to a simplified set of equations, depending only on the parameter, λ = √ δ / ∆ in leading order of the expansions. Keeping leading order in ∆ is equivalent to the infrared limit, in which only relevant and marginal terms contribute to the equations of motion. The number of axions in the star is uniquely determined by λ. Numerical solutions are found in a wide range of λ. At small λ the mass and radius of the axion star rise linearly with λ. While at larger λ the radius of the star continues to rise, the mass of the star, M , attains a maximum at λ max 0.58. All stars are unstable for λ > λ max . We discuss the relationship of our results to current observational constraints on dark matter and the phenomenology of Fast Radio Bursts.

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Section: Analytic Approximations To the Physical Parameters Of Axion mentioning

confidence: 81%

Section: Axion Field Dynamics In the Condensed Statementioning

confidence: 99%

Section: Jhep03(2015)080mentioning

confidence: 99%

Section: Analytic Approximations To the Physical Parameters Of Axion mentioning

confidence: 99%

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Axion stars in the infrared limit

Eby

Surányi

Vaz

et al. 2015

J. High Energ. Phys.

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“…The masses of weakly bound axion stars have been computed previously [23,24], and they are bounded above by gravitational stability [24][25][26]. Axion stars which exceed this maximum mass M c have a fate which remains an open question.…”

Section: Introductionmentioning

confidence: 99%

Collapse of axion stars

Eby

Leembruggen

Surányi

et al. 2016

J. High Energ. Phys.

117

191

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Axion stars, gravitationally bound states of low-energy axion particles, have a maximum mass allowed by gravitational stability. Weakly bound states obtaining this maximum mass have sufficiently large radii such that they are dilute, and as a result, they are well described by a leading-order expansion of the axion potential. Heavier states are susceptible to gravitational collapse. Inclusion of higher-order interactions, present in the full potential, can give qualitatively different results in the analysis of collapsing heavy states, as compared to the leading-order expansion. In this work, we find that collapsing axion stars are stabilized by repulsive interactions present in the full potential, providing evidence that such objects do not form black holes. In the last moments of collapse, the binding energy of the axion star grows rapidly, and we provide evidence that a large amount of its energy is lost through rapid emission of relativistic axions.

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What Can a GNOME Do? Search Targets for the Global Network of Optical Magnetometers for Exotic Physics Searches

Afach,

Aybas Tumturk,

Bekker

et al. 2023

Annalen der Physik

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Numerous observations suggest that there exist undiscovered beyond‐the‐standard‐model particles and fields. Because of their unknown nature, these exotic particles and fields could interact with standard model particles in many different ways and assume a variety of possible configurations. Here, an overview of the global network of optical magnetometers for exotic physics searches (GNOME), the ongoing experimental program designed to test a wide range of exotic physics scenarios, is presented. The GNOME experiment utilizes a worldwide network of shielded atomic magnetometers (and, more recently, comagnetometers) to search for spatially and temporally correlated signals due to torques on atomic spins from exotic fields of astrophysical origin. The temporal characteristics of a variety of possible signals currently under investigation such as those from topological defect dark matter (axion‐like particle domain walls), axion‐like particle stars, solitons of complex‐valued scalar fields (Q‐balls), stochastic fluctuations of bosonic dark matter fields, a solar axion‐like particle halo, and bursts of ultralight bosonic fields produced by cataclysmic astrophysical events such as binary black hole mergers are surveyed.

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Self-gravitating system made of axions

Cited by 121 publications

References 44 publications

Axion stars in the infrared limit

Axion stars in the infrared limit

Collapse of axion stars

What Can a GNOME Do? Search Targets for the Global Network of Optical Magnetometers for Exotic Physics Searches

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