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The accreting compact objects in most of ultraluminous X-ray sources (ULXs)are likely to be neutron stars rather than black holes as suggested by therecent detection of periodic pulsations from some of these sources located inneighboring galaxies and one ULX that has hitherto been discovered in our owngalaxy. As a member of the ULX family, NGC 300 ULX1 is a new pulsating ULX(PULX) spinning up at substantially high rates compared with other PULXs. Inthis paper, the strength of the magnetic field on the surface of the neutronstar is inferred from the energy of the cyclotron absorption line detected inthe pulsed X-ray spectrum of NGC 300 ULX1 and the plausible ranges for theneutron-star mass and beaming fraction are estimated using the observed spinperiod and period derivative of the pulsar and the measured X-ray flux of thesource. Our analysis favors proton cyclotron resonance scattering as a viablemechanism to account for both the observed cyclotron energy and high spin-uprates provided that the absorption line is generated close to the surface ofthe neutron star.

On the Mass and Magnetic Field of the Neutron Star in the Ultraluminous X-Ray Source NGC 300 ULX1