Stability and Formation of Solitonic Boson Stars
Abstract
We extend a previous study of the radial stability of solitonic boson stars by nonlinearly evolving them under aspherical perturbations, and by studying their formation from the collapse of scalar clouds. We focus in particular on models previously identified as radially stable, despite having positive binding energy, which ordinarily suggests that dispersion of all scalar matter is energetically preferred. A mode analysis of our 3+1 evolutions produces no evidence for the presence of a non-radial instability in any radially stable model, including those with positive binding energy. However, we do find evidence that such models do not generically form via gravitational cooling. We also find that it is possible to form another kind of compact object, which undergoes long-lasting radial oscillations and hence cannot be described as a stationary boson star. These objects may be characterized, we suggest, by energetically favoured multi-oscillating solutions to the Einstein-Klein-Gordon equations, present in certain regions of the parameter space.
Related
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- Vanishing Island: Spectral Criticality in Boson Stars
- Timing-Window Mechanism for Chain-Like Transients in Collisions of Radially Excited Boson Stars
- The Dynamical Instability of Rotating Boson Stars
- Relative-Phase Control of Common-Bridge Survival in Collisions of Radially Excited Boson Stars
BibTeX
@misc{marks2026stability,
title = {{Stability and Formation of Solitonic Boson Stars}},
author = {Gareth Arturo Marks},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2609.30021},
eprint = {2609.30021},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.30021},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Stability and Formation of Solitonic Boson Stars
AU - Gareth Arturo Marks
PY - 2026
DA - 2026/10/14
PB - arXiv
DO - 10.48550/arxiv.2609.30021
UR - https://arxiv.org/abs/2609.30021
AB - We extend a previous study of the radial stability of solitonic boson stars by nonlinearly evolving them under aspherical perturbations, and by studying their formation from the collapse of scalar clouds. We focus in particular on models previously identified as radially stable, despite having positive binding energy, which ordinarily suggests that dispersion of all scalar matter is energetically preferred. A mode analysis of our 3+1 evolutions produces no evidence for the presence of a non-radial instability in any radially stable model, including those with positive binding energy. However, we do find evidence that such models do not generically form via gravitational cooling. We also find that it is possible to form another kind of compact object, which undergoes long-lasting radial oscillations and hence cannot be described as a stationary boson star. These objects may be characterized, we suggest, by energetically favoured multi-oscillating solutions to the Einstein-Klein-Gordon equations, present in certain regions of the parameter space.
ER -