We work out domain walls in neutron 3 P2 superfluids realized in the core of neutron stars. Adopting the Ginzburg-Landau 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.
I. INTRODUCTIONDomain walls or kinks are solitonic objects separating two discrete vacua or ground states of a system [1-3] and play important roles in various subjects of physics from condensed matter physics [4] to cosmology [5] and supersymmetric field theories [6]. They are often created in phase transitions associated with symmetry breakings [7]. In cosmology, if they appear at a phase transition in the early Universe, then the so-called domain wall problem occurs [5]: the domain wall energy dominates Universe to make it collapse. In helium superfluids, such domain walls are created in a similar manner, thereby simulating cosmological phase transitions [8]. Here, we focus on domain walls in neutron stars, more precisely those in nuclear matter.Neutron stars are compact stars under extreme conditions, thereby serving as astrophysical laboratories for studying nuclear matter at high density, under rapid rotation and with a strong magnetic field (see Refs. [9,10] for recent reviews). The recent progresses in astrophysical observations promote us to study the neutron stars more precisely, such as the recent reports on massive neutron stars whose masses are almost twice as large as the solar mass [11,12] and the gravitational waves from a binary neutron star merger [13].Inside neutron stars, one of the most important key ingredients for understanding the inner structure is neutron superfluidity and proton superconductivity (see for recent reviews). Since the superfluid and superconducting components can alter excitation modes at low energy from the normal phase, their existence can affect several * yasuis@keio.jp † nitta(at)phys-h.keio.ac.jp arXiv:1907.12843v1 [nucl-th] 30 Jul 20191 Although the 1 S 0 superfluidity at low density was proposed in Ref. [28], it was shown in Ref.[29] that this channel turns to be repulsive due...