Heavy scalar fields in neutron stars form interior shell-localized profiles that reshape the effective equation of state and break the I-Q relation while remaining hidden from binary pulsar observations.
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Neural networks trained on noise-free post-merger spectra outperform linear regression baselines at predicting neutron-star mass, quadrupolar tidal deformability, and mass-radius slope from numerical-relativity catalogs.
Linear coupling and rotation in scalar-tensor theories produce a complex phase transition landscape for scalarized neutron stars, with rotation increasing critical masses and Landau theory revealing overlooked solution branches.
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Phase transition structure of scalarized neutron stars: the effect of rotation and linear coupling
Linear coupling and rotation in scalar-tensor theories produce a complex phase transition landscape for scalarized neutron stars, with rotation increasing critical masses and Landau theory revealing overlooked solution branches.