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We report the discovery of 105-ms X-ray pulsations from the compact centralobject (CCO) in the supernova remnant Kes 79 using data acquired with theNewton X-Ray Multi-Mirror Mission. Two observations of the pulsar taken 6 daysapart yield an upper limit on its spin-down rate of dP/dt < 7E-14 s/s and noevidence for binary orbital motion. The implied energy loss rate is dE/dt <2E36 ergs/s, surface magnetic field strength is B_p < 3E12 G, and spin-down ageis t > 24 kyr. The latter exceeds the remnant's estimated age, suggesting thatthe pulsar was born spinning near its current period. The X-ray spectrum of PSRJ1852+0040 is best characterized by a blackbody model of temperature kT_BB =0.44 +/- 0.03 keV, radius R_BB approx. 0.9 km, and L_bol = 3.7E33 ergs/s at d =7.1 kpc. The sinusoidal light curve is modulated with a pulsed fraction of>45%, suggestive of a small hot spot on the surface of the rotating neutronstar. The lack of a discernible pulsar wind nebula is consistent with aninterpretation of PSR J1852+0040 as a rotation-powered pulsar whose spin-downluminosity falls below the empirical threshold for generating bright windnebulae, dE/dt_c approx. 4E36 ergs/s. The age discrepancy implies that itsdE/dt has always been below dE/dt_c, perhaps a distinguishing property of theCCOs. Alternatively, the X-ray spectrum of PSR J1852+0040 suggests alow-luminosity AXP, but the weak inferred B_p field is incompatible with amagnetar theory of its X-ray luminosity. So far, we cannot exclude accretionfrom a fall-back disk. The ordinary spin parameters discovered from PSRJ1852+0040 highlight the difficulty that existing theories of isolated neutronstars have in explaining the high luminosities and temperatures of CCO thermalX-ray spectra.Comment: 8 pages, 4 Figues. Latex, emulateapj.sty. To appear in the  Astrophysical Journa

Discovery of a 105 ms X‐Ray Pulsar in Kesteven 79: On the Nature of Compact Central Objects in Supernova Remnants