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Many classes of extended scalar-tensor theories predict that dynamicalinstabilities can take place at high energies, leading to the formation ofscalarized neutron stars. Depending on the theory parameters, stars in ascalarized state can form a solution-space branch that shares a lot ofsimilarities with the so-called mass twins in general relativity appearing forequations of state containing first-order phase transitions. Members of thisscalarized branch have a lower maximum mass and central energy density comparedto Einstein ones. In such cases, a scalarized star could potentiallyover-accrete beyond the critical mass limit, thus triggering a gravitationalphase transition where the star sheds its scalar hair and migrates over to itsnon-scalarized counterpart. Such an event resembles, though is distinct from, anuclear or thermodynamic phase transition. We dynamically track a gravitationaltransition by first constructing hydrostatic, scalarized equilibria forrealistic equations of state, and then allowing additional material to fallonto the stellar surface. The resulting bursts of monopolar radiation aredispersively-stretched to form a quasi-continuous signal that persists fordecades, carrying strains of order $\gtrsim10^{-22} (\text{kpc}/L)^{3/2} \text{Hz}^{-1/2}$ at frequencies of $\lesssim300 \text{ Hz}$, detectable with theexisting interferometer network out to distances of $L\lesssim10 \text{ kpc}$,and out to a few hundred kpc with the inclusion of the Einstein Telescope.Electromagnetic signatures of such events, involving gamma-ray and neutrinobursts, are also considered.

Gravitational waves from accretion-induced descalarization in massive scalar-tensor theory