A first-principles energy-function calculation determines the quartic coefficient b0 whose sign sets the order of the spontaneous-scalarization phase transition in scalar-tensor neutron stars.
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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.
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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Underlying mechanisms of phase transitions in scalar-tensor theories
A first-principles energy-function calculation determines the quartic coefficient b0 whose sign sets the order of the spontaneous-scalarization phase transition in scalar-tensor neutron stars.
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Donutization Inside Neutron Stars: Shell-Localized Scalar Fields
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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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.