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Brussel-Montreal density functional has been designed to describe accurately nuclear matter in neutron stars. Hence, the fitting was done not only using experimental nuclear data (as it is usually done) but also theoretical results for many-body calculations (for example pairing gaps).
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See [slides by Nicolas Chamel](https://theory.gsi.de/hirschegg/2017/talks/Thu/Chamel.pdf)
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In the following articles one can find more details about the functional family:
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* [Nicolas Chamel, Stéphane Goriely, and JM Pearson. ‘Further explorations of skyrme–hartree–fock–bogoliubov mass formulas. ix: Constraint of pairing force to 1s0 neutron-matter gap’. Nuclear Physics A 812 (2008), 72](https://www.sciencedirect.com/science/article/abs/pii/S0375947408006921)
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* [PhysRevC.80.065804](https://link.aps.org/doi/10.1103/PhysRevC.80.065804)
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* [PhysRevC.82.014313](https://link.aps.org/doi/10.1103/PhysRevC.82.014313)
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* ‘Spin and spin-isospin instabilities in asymmetric nuclear matter at zero and finite temperatures using skyrme functionals’. Physical Review C 82 (2010), 045804
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* [PhysRevC.85.035801](https://link.aps.org/doi/10.1103/PhysRevC.85.035801)
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* [Nicolas Chamel, Stéphane Goriely, and John Michael Pearson. ‘Pairing:
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From atomic nuclei to neutron star crusts’. In ‘Fifty Years of Nuclear
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BCS: Pairing in Finite Systems’](https://doi.org/10.1142/9789814412490_0021)
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* [PhysRevLett.102.152503](https://link.aps.org/doi/10.1103/PhysRevLett.102.152503)
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* [PhysRevC.93.034337](https://link.aps.org/doi/10.1103/PhysRevC.93.034337)
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