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The accretion-powered (non-X-ray burst) pulsations of XTE J1814-338 aremodeled to determine neutron star parameters and their uncertainties. The modelis a rotating circular hot spot and includes: (1) an isotropic blackbodyspectral component; (2) an anisotropic Comptonized spectral component; (3)relativistic time-delays and light-bending; and (4) the oblate shape of thestar due to rotation. This model is the simplest possible model that isconsistent with the data. The resulting best-fit parameters of the model favorstiff equations of state, as can be seen from the 3-sigma allowed regions inthe mass-radius diagram. We analyzed all data combined from a 23 day period ofthe 2003 outburst, and separately analyzed data from 2 days of the outburst.The allowed mass-radius regions for both cases only allow equations of state(EOS) that are stiffer than EOS APR (Akmal et al. 1998), consistent with thelarge mass that has been inferred for the pulsar NGC 6440B (Freire et al.2008). The stiff EOS inferred by this analysis is not compatible with the softEOS inferred from a similar analysis of SAX J1808.

Constraints on the Properties of the Neutron Star XTE J1814-338 from Pulse Shape Models