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Relativistic Stellar Oscillations from Ultralight Dark Matter
Abstract
Ultra-light dark matter, composed of bosons behaving as classical waves, can resonantly excite stellar oscillations. In this work, we investigate this phenomenon in relativistic stars, showing that ℓ=0 fluid modes can be excited. We derive a framework for calculating the mode amplitude and apply it to neutron stars to predict the associated surface temperature fluctuations; the resulting signal lies beyond current observational sensitivities. We discuss prospects for extending this approach to other compact objects.
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BibTeX
@misc{oishi2026relativistic,
title = {{Relativistic Stellar Oscillations from Ultralight Dark Matter}},
author = {Shanae Oishi and Christopher Reyes and Jeremy Sakstein},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.19500},
eprint = {2609.19500},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.19500},
}
RIS
TY - UNPB
TI - Relativistic Stellar Oscillations from Ultralight Dark Matter
AU - Shanae Oishi
AU - Christopher Reyes
AU - Jeremy Sakstein
PY - 2026
DA - 2026/09/16
PB - arXiv
DO - 10.48550/arxiv.2609.19500
UR - https://arxiv.org/abs/2609.19500
AB - Ultra-light dark matter, composed of bosons behaving as classical waves, can resonantly excite stellar oscillations. In this work, we investigate this phenomenon in relativistic stars, showing that ℓ=0 fluid modes can be excited. We derive a framework for calculating the mode amplitude and apply it to neutron stars to predict the associated surface temperature fluctuations; the resulting signal lies beyond current observational sensitivities. We discuss prospects for extending this approach to other compact objects.
ER -