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Recent observations of the central compact object in the Kesteven 79supernova remnant show that this neutron star (NS) has a weak dipole magneticfield (a few x 10^{10} G) but an anomalously large (~ 64%) pulse fraction inits surface X-ray emission. We explore the idea that a substantial sub-surfacemagnetic field exists in the NS crust, which produces diffuse hot spots on thestellar surface due to anisotropic heat conduction, and gives rise to theobserved X-ray pulsation. We develop a general-purpose method, termed"Temperature Template with Full Transport" (TTFT), that computes the syntheticpulse profile of surface X-ray emission from NSs with arbitrary magnetic fieldand surface temperature distributions, taking into account magnetic atmosphereopacities, beam pattern, vacuum polarization, and gravitational light bending.We show that a crustal toroidal magnetic field of order a few x 10^{14} G orhigher, varying smoothly across the crust, can produce sufficiently distinctsurface hot spots to generate the observed pulse fraction in the Kes 79 NS.This result suggests that substantial sub-surface magnetic fields, muchstronger than the "visible" dipole fields, may be buried in the crusts of someyoung NSs, and such hidden magnetic fields can play an important role in theirobservational manifestations. The general TTFT tool we have developed can alsobe used for studying radiation from other magnetic NSs.

The Hidden Magnetic Field of The Young Neutron Star in Kesteven 79