TY - JOUR

T1 - Domain walls in neutron P2 3 superfluids in neutron stars

AU - Yasui, Shigehiro

AU - Nitta, Muneto

PY - 2020/1/21

Y1 - 2020/1/21

N2 - We work out domain walls in neutron P23 superfluids realized in the core of neutron stars. Adopting the Ginzburg-Landau (GL) theory as a bosonic low-energy effective theory, we consider configurations of domain walls interpolating ground states, i.e., the uniaxial nematic (UN), D2-biaxial nematic (D2-BN), and D4-biaxial nematic (D4-BN) phases in the presence of zero, small and large magnetic fields, respectively. We solve the Euler-Lagrange equation from the GL free energy density, and calculate surface energy densities of the domain walls. We find that one extra Nambu-Goldstone mode is localized in the vicinity of a domain wall in the UN phase while a U(1) symmetry restores in the vicinity of one type of domain wall in the D2-BN phase and all domain walls in the D4-BN phase. Considering a pile of domain walls in the neutron stars, we find that the most stable configurations are domain walls perpendicular to the magnetic fields piled up in the direction along the magnetic fields in the D2-BN and D4-BN phases. We estimate the energy released from the deconstruction of the domain walls in the edge of a neutron star, and show that it can reach an astrophysical scale such as glitches in neutron stars.

AB - We work out domain walls in neutron P23 superfluids realized in the core of neutron stars. Adopting the Ginzburg-Landau (GL) theory as a bosonic low-energy effective theory, we consider configurations of domain walls interpolating ground states, i.e., the uniaxial nematic (UN), D2-biaxial nematic (D2-BN), and D4-biaxial nematic (D4-BN) phases in the presence of zero, small and large magnetic fields, respectively. We solve the Euler-Lagrange equation from the GL free energy density, and calculate surface energy densities of the domain walls. We find that one extra Nambu-Goldstone mode is localized in the vicinity of a domain wall in the UN phase while a U(1) symmetry restores in the vicinity of one type of domain wall in the D2-BN phase and all domain walls in the D4-BN phase. Considering a pile of domain walls in the neutron stars, we find that the most stable configurations are domain walls perpendicular to the magnetic fields piled up in the direction along the magnetic fields in the D2-BN and D4-BN phases. We estimate the energy released from the deconstruction of the domain walls in the edge of a neutron star, and show that it can reach an astrophysical scale such as glitches in neutron stars.

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U2 - 10.1103/PhysRevC.101.015207

DO - 10.1103/PhysRevC.101.015207

M3 - Article

AN - SCOPUS:85078866158

VL - 101

JO - Physical Review C

JF - Physical Review C

SN - 2469-9985

IS - 1

M1 - 015207

ER -