Neutron stars (NSs) provide an extraordinary natural laboratory to explore superconductivity and superfluidity under extreme conditions—high density, strong magnetic fields, and ultra-low temperatures. Decades of theoretical work have suggested the presence of these quantum states in NS interiors, and observational hints, such as the rapid cooling of Cassiopeia A, support this idea. Why superconductivity arises in NSs As neutron stars cool below 𝑇 ∼ 10 9   K T∼10 9 K, primarily via neutrino emission from beta decay, the degenerate proton fluid can undergo BCS-type pairing and become superconducting. This occurs in a background of frozen-in magnetic fields, often reaching 𝐵 ∼ 10 15 − 10 16   G B∼10 15 −10 16 G in the core, particularly in magnetars. Unlike lab superconductors (where electrons pair via phonon interactions in a lattice), NSs lack a lattice. Instead, protons form Cooper pairs via the attractive tail of the strong nuclear force. Electrons in NSs remain unpaired due to their ultrarelativistic nature and extremely low 𝑇 𝑐 T c ​ values. The resulting system exhibits finite-temperature superconductivity with 𝑇 / 𝑇 𝐹 ∼ 10 − 3 T/T F ​ ∼10 −3 , inaccessible on Earth. How NS superconductivity differs from terrestrial cases No phonon mediation; pairing is purely nuclear. No lattice structure; hence, field expulsion behaves differently. Extremely high electrical conductivity delays magnetic field expulsion, making Meissner effect non-ideal. Superconductivity can be type-I or type-II, depending on local microphysical parameters and field strength. Two distinct superconducting regimes (see figure) The superconducting behavior depends on the Ginzburg-Landau parameter 𝜅 = 𝜆 / 𝜉 κ=λ/ξ: Type I ( 𝜅 < 1 / 2 κ<1/ 2 ​ ): The magnetic field is ideally expelled (Meissner effect) below 𝐻 𝑐 𝑚 H cm ​ , but in NSs, this process is inefficient. The magnetic field remains trapped or discontinuously distributed in layered domains. Type II ( 𝜅 > 1 / 2 κ>1/ 2 ​ ): The field partially penetrates the superconductor between 𝐻 𝑐 1 H c1 ​ and 𝐻 𝑐 2 H c2 ​ as quantized flux tubes, forming an ordered lattice. These tubes enhance internal magnetic stress and deform the star—key for gravitational wave emission. Key questions our study addresses (see figure): Is the proton superconductor in NSs type I or type II? Where in the star does superconductivity exist—outer core or inner core? What is the geometry of the superconducting regions? Can we observe its effects indirectly, e.g., through gravitational waves? Our contribution We conduct the first 2D general relativistic study of superconductivity in magnetars with toroidal fields, using the XNS code to solve the Einstein-Maxwell equations with: Realistic EOS for nuclear matter, Temperature-dependent proton pairing gaps, Finite magnetic field strengths up to 10 16   G 10 16 G. This enables us to map out type-I, type-II, and non-superconducting zones, including novel torus-shaped normal regions, and track their dependence on stellar mass, field configuration, and thermal evolution. Broader impact Our work has implications for the detectability of continuous gravitational waves from isolated neutron stars. In superconducting NSs, magnetic stresses and resulting ellipticities are significantly enhanced—making gravitational wave strain potentially observable in next-generation detectors. Thus, NS superconductivity may be indirectly confirmed via gravitational wave astronomy.