Magnetars are neutron stars with extreme magnetic fields. In DRUMS, the neutron star core is a dense superfluid coupled to the cubic magnetic substrate:
Phase coherence in the core mediates both rotational dynamics and magnetic field alignment.
The magnetic field arises from superfluid vortices aligned with the substrate:
Here \(n_i\) counts quantized vortices, \(m_n\) is neutron mass, and \(\hat{z}_i\) aligns with local cubic lattice axes.
For vortex density \(n_v\) and superfluid core radius \(R_{core}\):
This reproduces observed fields \(10^{14}–10^{15}\) G.
Superfluid vortices mediate angular momentum exchange, producing spin-down rates:
Where \(\Omega\) is rotation rate, \(I\) moment of inertia, consistent with magnetar periods.
Sudden rearrangements of vortices trigger high-energy bursts:
Phase discontinuities in the superfluid correspond to observed magnetar flares and soft gamma repeaters.
The magnetar crust interacts with the superfluid core:
This explains glitches and sudden spin changes.
Magnetar evolution is governed by decay of superfluid vortices and phase relaxation:
Where \(\tau_{vortex}\) is characteristic vortex decay timescale (~10^4–10^5 years).
Within the DRUMS framework, magnetars are fully explained as: