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We explore the prospects for identifying differences in simulatedgravitational-wave signals of binary neutron star (BNS) mergers associated withthe way thermal effects are incorporated in the numerical-relativity modelling.We consider a hybrid approach in which the equation of state (EoS) comprises acold, zero temperature, piecewise-polytropic part and a thermal part describedby an ideal gas, and a tabulated approach based on self-consistent,microphysical, finite-temperature EoS. We use time-domain waveformscorresponding to BNS merger simulations with four different EoS. Those areinjected into Gaussian noise given by the sensitivity of the third-generationdetector Einstein Telescope and reconstructed using BayesWave, a Bayesiandata-analysis algorithm that recovers the signals through a model-agnosticapproach. The two representations of thermal effects result in frequency shiftsof the dominant peaks in the spectra of the post-merger signals, for both thequadrupole fundamental mode and the late-time inertial modes. For some of theEoS investigated those differences are large enough to be told apart,especially in the early post-merger phase when the signal amplitude is theloudest.

Identifying thermal effects in neutron star merger remnants with model-agnostic waveform reconstructions and third-generation detectors