Unified picture of Q-balls and boson stars via catastrophe theory

Abstract

We make an analysis of Q-balls and boson stars using catastrophe theory, as an extension of the previous work on Q-balls in flat spacetime. We adopt the potential $V_3(\varphi )=\frac{m^2}{2}{\varphi }^2-\mu {\varphi }^3+\lambda {\varphi }^4$ for Q-balls and that with $\mu =0$ for boson stars. For solutions with $|g^{rr}-1|\sim 1$ at its peak, stability of Q-balls has been lost regardless of the potential parameters. As a result, phase relations, such as a Q-ball charge versus a total Hamiltonian energy, approach those of boson stars, which tell us an unified picture of Q-balls and boson stars.

arXiv comment10 pages, 13 figures

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• Boson Stars and Oscillatons: A Review
• Models of rotating boson stars and geodesics around them: new type of orbits
• Stable Phases of Boson Stars
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• Compact Boson Stars
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• Compact (A)dS Boson Stars and Shells
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• Q-tubes and Q-crusts
• Self-interacting boson stars with a single Killing vector field in Anti-de Sitter
• Scalaroca stars: coupled scalar-Proca solitons
• What are universal features of gravitating Q-balls?
• Unified pictures of Q-balls and Q-tubes
• What happens to Q-balls if $Q$ is so large?
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