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tokens: within the time span of 21–39 days after the latest outburst onset (in the absence of intense bursts), Younes et al. ( 2020b ) precisely measured a much higher spin-down rate of 3.9 × 10 −11 s s −1 . This might suggest a hysteresis in the dynamical response in these highly magnetized systems that is accompanied by changes in burst activation. The polar magnetic field strength inferred for a vacuum dipole approximation (i.e., ) of SGR J1935+2154 is about 4.4 × 10 14 G. However, our X-ray spectral modeling of the persistent emission with the STEMS3D model, which includes radiative propagation in extremely magnetized settings, yielded a local surface magnetic field strength of 9.6 × 10 14 G. This difference is not surprising since the spin-down estimate applies to the global field configuration, and can be modified by plasma loading of the magnetosphere (Harding et al. 1999 ). Nevertheless, the surface magnetic field strength being considerably larger than the inferred value suggests that there may be multipolar magnetic topology, where local field strengths are much larger than the dipolar ones. Such a circumstance was observed in SGR 0418+5729, the first “low-dipole field” magnetar. Its magnetic field strength inferred from its spin parameters is 6 × 10 12 G (Rea et al. 2010 ). Güver et al. ( 2011 ) modeled the XMM-Newton spectrum of SGR 0418−5729 with the STEMS atmospheric emission model and obtained ∼ 10 14 G for the surface magnetic field strength. They proposed a dominant nondipolar magnetic field structure for SGR 0418−5729, a picture that is consistent with the discovery of a variable proton cyclotron absorption feature in later XMM-Newton observations (Tiengo et al. 2013 ). A significant multipolar magnetic configuration for SGR J1935+2154 is also supported by the complexity of its energy-dependent pulse profiles. Its low-energy X-ray pulse profile is dominated by a broad structure with a phase width of around 0.7–0.8. However, minor structures become pronounced above ∼3 keV, in the absence of bright persistent X-ray emission ( kT = 0.5 keV) from the surface of the neutron star. The BB+BB spectral fits indicate that this putatively hotter portion emanates from smaller regions, less than ∼0.2 km in size, and perhaps analogous to multipolar field components that are observed from small regions on the Sun. These structured pulse profiles contrast the comparatively simple two-peaked forms observed for active outburst phases in another magnetar, 1RXS J170849.0−400910, which can be attributed to antipodal polar hot zones in a dipole field configuration (Younes et al. 2020a ). Extension of the pulse profile analysis of Younes et al. ( 2020a ) to treat broader surface temperature profiles in magnetic colatitude is unlikely to generate the abrupt rises and falls in consecutive phase bins evident above ∼3 keV in Figure 1 . We suggest that strong temperature gradients in magnetic longitude are also required to reproduce the observed