Abstract
Nuclear pasta, that is an inhomogeneous distribution of nuclear matter characterised by non-spherical clustered structures, is expected to occur in a narrow spatial region at the bottom of the inner crust of neutron stars, but the width of the pasta layer is strongly model dependent. In the framework of a compressible liquid-drop model, we use Bayesian inference to analyse the constraints on the sub-saturation energy functional and surface tension imposed by both ab-initio chiral perturbation theory calculations and experimental measurements of nuclear masses. The posterior models are used to obtain general predictions for the crust-pasta and pasta-core transition with controlled uncertainties. A correlation study allows us to extract the most influential parameters for the calculation of the pasta phases. The important role of high-order empirical parameters and of the surface tension is underlined.
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This manuscript has no associated data or the data will not be deposited. [Authors’ comment: Data generated during this study are contained in this published article.]
Notes
In this section and the following ones, the surface parameter p is systematically included in the \(\mathbf {X}\) parameter set as an additional independent parameter, with a flat prior distribution as given in Table 1.
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Acknowledgements
This work has been partially supported by the IN2P3 Master Project NewMAC and the CNRS International Research Project (IRP) “Origine des éléments lourds dans l’univers: Astres Compacts et Nucléosynthèse (ACNu)”.
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Dinh Thi, H., Fantina, A.F. & Gulminelli, F. The effect of the energy functional on the pasta-phase properties of catalysed neutron stars. Eur. Phys. J. A 57, 296 (2021). https://doi.org/10.1140/epja/s10050-021-00605-6
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DOI: https://doi.org/10.1140/epja/s10050-021-00605-6