Bayesian inference of the crust–core transition density via the neutron-star radius and neutron-skin thickness data
Author:
Publisher
Springer Science and Business Media LLC
Subject
Nuclear Energy and Engineering,Nuclear and High Energy Physics
Link
https://link.springer.com/content/pdf/10.1007/s41365-023-01239-7.pdf
Reference46 articles.
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2. N. Paar, C.C. Moustakidis, T. Marketin et al., Neutron star structure and collective excitations of finite nuclei. Phys. Rev. C 90, 011304 (2014). https://doi.org/10.1103/PhysRevC.90.011304
3. M. Centelles, X. Roca-Maza, X. Vinas et al., Nuclear symmetry energy probed by neutron skin thickness of nuclei. Phys. Rev. Lett. 102, 122502 (2009). https://doi.org/10.1103/PhysRevLett.102.122502
4. C. Horowitz, J. Piekarewicz, Neutron star structure and the neutron radius of $$^{208}$$pb. Phys. Rev. Lett. 86, 5647 (2001). https://doi.org/10.1103/PhysRevLett.86.5647
5. L. Tsaloukidis, C. Margaritis, C.C. Moustakidis, Effects of the equation of state on the core-crust interface of slowly rotating neutron stars. Phys. Rev. C 99, 015803 (2019). https://doi.org/10.1103/PhysRevC.99.015803
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