much better description of the data ([$\chi^2_r$]{}of 1.11 for 628), yielding a blackbody with $0.233\pm0.003$keV and $318\pm5$km for the soft excess, and $1.83\pm0.03$keV and $14.7\pm0.3$km for the higher energy emission (presumably the photosphere). Some structure still remained in the residuals, most prominently at 1.0keV and 6.5keV. The fit was significantly improved ([$\chi^2_r$]{}of 1.07 for 624 dof) by adding a `diskline` component [@Fabian1989] at $6.7_{-0.3}^{+0.1}$keV, along with a Gaussian line at $1.05\pm0.02$keV. The signal strength of the `diskline` was insufficient to reliably constrain the disk radius and inclination, giving respective limits of $<13\,r_g$ and $>65\arcdeg$. Instead, we fixed the inner radius to $11\,r_g$, which is the approximate magnetospheric radius [@Bult2015b], and the inclination to $65\arcdeg$, which is within the range allowed by modelling of the FeK line in the persistent emission of [SAX J1808]{}. We further note that while this inclination is inconsistent with the $\leq30\arcdeg$ limit derived by @Galloway2006, a more sophisticated analysis of the same burst data yield $69_{-2}^{+4}\arcdeg$ [@Goodwin2019]. With these parameters held constant, we obtained a line normalization of $0.62\pm0.16$[[ph[cm$^{-2}$]{}[s$^{-1}$]{}]{}]{}. Meanwhile, the 1[[keV]{}]{}Gaussian line had a normalization of $0.27\pm0.07$[[ph[cm$^{-2}$]{}[s$^{-1}$]{}]{}]{}and standard deviation of $0.05_{-0.02}^{+0.07}$keV.

In an attempt to apply a physical foundation to our modelling of these data, 