Skip to content
DraconiticResearch
Search Sources API
203,234 studies31 sourcesUpdated 33 min ago
Peer-reviewedCC BYEuropean physical journal plus

Probing flavour deconstruction via primordial gravitational waves.

  • Noemi Fabri1
  • Gino Isidori1
  • Davide Racco1,2,3
  1. 1Physik-Institut, Universität Zürich, Winterthurerstrasse 190, 8057 Zürich, Switzerland.
  2. 2Institut für Theoretische Physik, ETH Zürich, Wolfgang-Pauli-Str. 27, 8093 Zürich, Switzerland.
  3. 3Stanford Institute for Theoretical Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
Read full textPDFDOICite

Abstract

We study the production of primordial gravitational waves (GWs) from first-order phase transitions (FOPTs) in extensions of the Standard Model based on Flavour Deconstruction (FD). The link fields inherent to FD generically form a rich scalar sector, with sizeable couplings at the TeV scale, providing natural conditions for strong FOPTs and correspondingly large GW emission. We identify the key parameters controlling the GW spectrum and enabling its detection at future GW observatories. In particular, we find that while FD scenarios can yield detectable signals, the resulting spectra typically peak at higher frequencies than the millihertz range. As a consequence, a positive observation at LISA is possible but not guaranteed, while the signal falls in the range of mid-band proposals, making FD models an intriguing target for upcoming GW searches.

Related

  1. Probing Helical Primordial Magnetic Fields via Chiral Gravitational Waves in the LISA-TAIJI Network
    Kazuya Furusawa, Hiroyuki Tashiro
    arXivPreprintCC BY 4.0Full textCosmologyGravitation & general relativityarXiv
  2. Reconstructing stochastic gravitational-wave signals from flavour deconstruction with LISA
    Noemi Fabri, Raphael Bertrand-Delgado, Danny Laghi +1
    arXivPreprintCC BY 4.0Full textCosmologyGravitation & general relativityarXiv
  3. Neutron Star--Primordial Black Hole Binaries: Dynamical Tides, Resonance Locking, and Gravitational Waves
    Isaac Legred, Nicolás Yunes
    arXivPreprintCC BY 4.0Full textHigh-energy astrophysicsGravitation & general relativityarXiv
  4. Primordial black holes and gravitational waves from aligned axion inflation
    Nadir Ijaz
    arXivPreprintarXiv licenceFull textCosmologyHigh-energy & particle physicsarXiv
  5. The fate of primordial gravitational waves during domain-wall domination
    Zhen-Min Zeng
    arXivPreprintCC BY-NC-SA 4.0Full textGravitation & general relativityarXiv

Cite

BibTeXRIS
BibTeX
@article{fabri2026probing,
  title = {{Probing flavour deconstruction via primordial gravitational waves.}},
  author = {Noemi Fabri and Gino Isidori and Davide Racco},
  journal = {European physical journal plus},
  year = {2026},
  month = oct,
  doi = {10.1140/epjp/s13360-026-08080-y},
  url = {https://europepmc.org/article/MED/42922901},
  note = {CC BY},
}
RIS
TY  - JOUR
TI  - Probing flavour deconstruction via primordial gravitational waves.
AU  - Noemi Fabri
AU  - Gino Isidori
AU  - Davide Racco
PY  - 2026
DA  - 2026/10/21
JO  - European physical journal plus
DO  - 10.1140/epjp/s13360-026-08080-y
UR  - https://europepmc.org/article/MED/42922901
AB  - We study the production of primordial gravitational waves (GWs) from first-order phase transitions (FOPTs) in extensions of the Standard Model based on Flavour Deconstruction (FD). The link fields inherent to FD generically form a rich scalar sector, with sizeable couplings at the TeV scale, providing natural conditions for strong FOPTs and correspondingly large GW emission. We identify the key parameters controlling the GW spectrum and enabling its detection at future GW observatories. In particular, we find that while FD scenarios can yield detectable signals, the resulting spectra typically peak at higher frequencies than the millihertz range. As a consequence, a positive observation at LISA is possible but not guaranteed, while the signal falls in the range of mid-band proposals, making FD models an intriguing target for upcoming GW searches.
SN  - 2190-5444
ER  -