Numerical simulations of eccentric Proca-star mergers show that relative phase between the stars controls post-merger fate and can generate odd-mode gravitational waves absent from black-hole mergers.
Bernuzzi, Neutron star merger remnants, General Rel- ativity and Gravitation 52, 108 (2020), arXiv:2004.06419 [astro-ph.HE]
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Lunar GW observatories can deliver weeks-to-months early warnings, 0.01 deg² localizations, and ~100 well-localized BNS events per year for GW170817-like sources, with multi-band networks yielding 0.1% mass-ratio and 1% distance precision.
A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
Comparative numerical study of radial modes in strange quark stars using CFL, interacting, and linear causal EOS shows all satisfy current mass-radius bounds and produce 4-7 kHz fundamental frequencies.
citing papers explorer
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Eccentric mergers of binary Proca stars
Numerical simulations of eccentric Proca-star mergers show that relative phase between the stars controls post-merger fate and can generate odd-mode gravitational waves absent from black-hole mergers.
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Binary Neutron Stars from the Moon: Early Warnings and Precision Science for the Artemis Era
Lunar GW observatories can deliver weeks-to-months early warnings, 0.01 deg² localizations, and ~100 well-localized BNS events per year for GW170817-like sources, with multi-band networks yielding 0.1% mass-ratio and 1% distance precision.
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Reconciling GW170817 and GW190814 with a Nonmonotonic Sound-Speed Equation of State
A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
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Radial oscillations of quark stars in light of current astrophysical constraints: A comparative study
Comparative numerical study of radial modes in strange quark stars using CFL, interacting, and linear causal EOS shows all satisfy current mass-radius bounds and produce 4-7 kHz fundamental frequencies.