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PreprintarXiv licencearXiv

Descalarization bursts from Galactic supramassive neutron stars: a kHz continuous-wave target

  • José Carlos Olvera M.
  • Daniela D. Doneva
  • Pablo Cerdá-Durán
  • José A. Font
  • Stoytcho S. Yazadjiev
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Abstract

In massive scalar-tensor gravity, a scalarized neutron star must shed its scalar hair as it collapses into a black hole. Using 3D simulations of a realistic rotating progenitor we show that dispersion stretches the emitted burst into a quasi-monochromatic signal in the kHz frequency range lasting >104 yr and amenable to continuous-wave methods. We find that detecting these signals in directed searches of supernova remnants without a central pulsar requires sensitivity depths of 233--762 Hz−1/2 with the A+-ET-CE detector network. We estimate up to ∼3 of these signals in transit at any observational epoch.

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Cite

BibTeXRIS
BibTeX
@misc{olvera2026descalarization,
  title = {{Descalarization bursts from Galactic supramassive neutron stars: a kHz continuous-wave target}},
  author = {José Carlos Olvera M. and Daniela D. Doneva and Pablo Cerdá-Durán and José A. Font and Stoytcho S. Yazadjiev},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.10728},
  eprint = {2610.10728},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.10728},
}
RIS
TY  - UNPB
TI  - Descalarization bursts from Galactic supramassive neutron stars: a kHz continuous-wave target
AU  - José Carlos Olvera M.
AU  - Daniela D. Doneva
AU  - Pablo Cerdá-Durán
AU  - José A. Font
AU  - Stoytcho S. Yazadjiev
PY  - 2026
DA  - 2026/10/07
PB  - arXiv
DO  - 10.48550/arxiv.2610.10728
UR  - https://arxiv.org/abs/2610.10728
AB  - In massive scalar-tensor gravity, a scalarized neutron star must shed its scalar hair as it collapses into a black hole. Using 3D simulations of a realistic rotating progenitor we show that dispersion stretches the emitted burst into a quasi-monochromatic signal in the kHz frequency range lasting >10^4 yr and amenable to continuous-wave methods. We find that detecting these signals in directed searches of supernova remnants without a central pulsar requires sensitivity depths of 233--762 Hz^−1/2 with the A+-ET-CE detector network. We estimate up to ∼3 of these signals in transit at any observational epoch.
ER  -