Speaker
Description
The presence of superfluidity in neutron star interiors can affect the cooling of neutron stars in intricate ways, enhancing certain mechanisms and suppressing others. Model calculations employing realistic nuclear potentials in Bardeen–Cooper–Schrieffer theory generally suggest the development of a 3P2–3F2 pairing gap, and therefore the presence of superfluidity in dense neutron star matter. Improved models that go beyond conventional mean-field calculations by including polarization effects suggest a suppression of the triplet gap.
In this work, we apply a large-scale summation of Feynman diagrams, including the class of parquet-diagrams plus important contributions outside the parquet class [1,2], for calculating effective pairing interactions and subsequently the superfluid gap in P-wave pairing in neutron matter. We employ realistic nucleon-nucleon interactions of the v8 type and perform calculations up to a Fermi momentum of 1.8 fm−1. We find that many-body correlations lead to a strong reduction of the spin-orbit interaction, and, therefore, to an almost complete suppression of the 3P2 and 3P2-3F2 gaps [2,3]. We also find pairing in 3P0 states. The strength of the pairing gap depends sensitively on the potential model employed. Our results for triplet pairing are relevant for assessing superfluidity in neutron star interiors, whose presence can affect substantially the cooling of neutron stars.
References:
[1] E. Krotscheck and J. Wang, Phys. Rev. C 101 (2020) 065804; Phys. Rev. C 102 (2020) 064305; Phys. Rev. C 103 (2021) 035808; Phys. Rev. C 105 (2022) 034345
[2] E. Krotscheck, P.P, J. Wang, Phys. Rev C 109 (2024) 015803
[3] E. Krotscheck, P.P., J. Wang, ApJ 955:76 (2023)
