Dilute and dense axion stars
Abstract
Axion stars are hypothetical objects formed of axions, obtained as localized and coherently oscillating solutions to their classical equation of motion. Depending on the value of the field amplitude at the core |$$\theta_0$$|≡ |$$\theta$$ (r=0), the equilibrium of the system arises from the balance of the kinetic pressure and either self-gravity or axion self-interactions. Starting from a general relativistic framework, we obtain the set of equations describing the configuration of the axion star, which we solve as a function of |$$\theta_0$$|. For small |$$\theta_0$$|≲1, we reproduce results previously obtained in the literature, and we provide arguments for the stability of such configurations in terms of first principles. We compare qualitative analytical results with a numerical calculation. For large amplitudes |$$\theta_0$$|≳1, the axion field probes the full non-harmonic QCD chiral potential and the axion star enters the $dense$ branch. Our numerical solutions show that in this latter regime the axions are relativistic, and that one should not use a single frequency approximation, as previously applied in the literature. We employ a multi-harmonic expansion to solve the relativistic equation for the axion field in the star, and demonstrate that higher modes cannot be neglected in the dense regime. We interpret the solutions in the dense regime as pseudo-breathers, and show that the life-time of such configurations is much smaller than any cosmological time scale.
- Authors:
- Publication Date:
- Research Org.:
- Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States); Univ. of Michigan, Ann Arbor, MI (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP); European Research Council (ERC); Swedish Research Council (SRC)
- OSTI Identifier:
- 1437800
- Alternate Identifier(s):
- OSTI ID: 1499285; OSTI ID: 1646990
- Grant/Contract Number:
- SC0012567; SC007859; 638-2013-8993; 335-2014-7424; FPA2015-65745-P; SFB-1258; 742104; SC0007859
- Resource Type:
- Published Article
- Journal Name:
- Physics Letters B
- Additional Journal Information:
- Journal Name: Physics Letters B Journal Volume: 777 Journal Issue: C; Journal ID: ISSN 0370-2693
- Publisher:
- Elsevier
- Country of Publication:
- Netherlands
- Language:
- English
- Subject:
- 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 79 ASTRONOMY AND ASTROPHYSICS
Citation Formats
Visinelli, Luca, Baum, Sebastian, Redondo, Javier, Freese, Katherine, and Wilczek, Frank. Dilute and dense axion stars. Netherlands: N. p., 2018.
Web. doi:10.1016/j.physletb.2017.12.010.
Visinelli, Luca, Baum, Sebastian, Redondo, Javier, Freese, Katherine, & Wilczek, Frank. Dilute and dense axion stars. Netherlands. https://doi.org/10.1016/j.physletb.2017.12.010
Visinelli, Luca, Baum, Sebastian, Redondo, Javier, Freese, Katherine, and Wilczek, Frank. Thu .
"Dilute and dense axion stars". Netherlands. https://doi.org/10.1016/j.physletb.2017.12.010.
@article{osti_1437800,
title = {Dilute and dense axion stars},
author = {Visinelli, Luca and Baum, Sebastian and Redondo, Javier and Freese, Katherine and Wilczek, Frank},
abstractNote = {Axion stars are hypothetical objects formed of axions, obtained as localized and coherently oscillating solutions to their classical equation of motion. Depending on the value of the field amplitude at the core |$\theta_0$|≡ |$\theta$ (r=0), the equilibrium of the system arises from the balance of the kinetic pressure and either self-gravity or axion self-interactions. Starting from a general relativistic framework, we obtain the set of equations describing the configuration of the axion star, which we solve as a function of |$\theta_0$|. For small |$\theta_0$|≲1, we reproduce results previously obtained in the literature, and we provide arguments for the stability of such configurations in terms of first principles. We compare qualitative analytical results with a numerical calculation. For large amplitudes |$\theta_0$|≳1, the axion field probes the full non-harmonic QCD chiral potential and the axion star enters the $dense$ branch. Our numerical solutions show that in this latter regime the axions are relativistic, and that one should not use a single frequency approximation, as previously applied in the literature. We employ a multi-harmonic expansion to solve the relativistic equation for the axion field in the star, and demonstrate that higher modes cannot be neglected in the dense regime. We interpret the solutions in the dense regime as pseudo-breathers, and show that the life-time of such configurations is much smaller than any cosmological time scale.},
doi = {10.1016/j.physletb.2017.12.010},
journal = {Physics Letters B},
number = C,
volume = 777,
place = {Netherlands},
year = {Thu Feb 01 00:00:00 EST 2018},
month = {Thu Feb 01 00:00:00 EST 2018}
}
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Cited by: 115 works
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Figures / Tables:
Table 1: The coefficients in the truncated series expansion of the chiral potential in Eq. (18), after the corrections described below Eq. (20) and for $z$ = 0.48.
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