include emission line components, giving in slightly poorer fit statistics. The resulting evolution in spectral parameters is shown in Figure \[fig:time resolved\].

The time resolved spectroscopy demonstrates that the hot ($\approx2$keV) blackbody in our model can be understood as the emission from a neutron star photosphere that undergoes PRE between $t\simeq1{{\rm\,s}\xspace}$ and $t\simeq13{{\rm\,s}\xspace}$. The radius expansion is moderate, reaching a maximum radius of $\approx15$km. The cool ($\approx0.2$keV) blackbody, on the other hand, maintains a stable temperature through the burst, with its emitting area closely tracking the evolution of the overall flux. This trend further supports the idea that the soft excess tracks an interaction between the burst emission and the neutron star environment, such as the disk reflection model discussed in Section \[sec:spectra\].

Considering the bolometric flux, we see that the burst emission reaches a stable peak of $(2.40\pm0.12){\ensuremath{\times 10^{-7}} }$[[erg[s$^{-1}$]{}[cm$^{-2}$]{}]{}]{}when the photosphere is at its largest extent. As the photosphere begins to contract, the flux begins to decrease. This cooling trend, however, is interrupted at $t\simeq15.5$. In the following $\approx3{{\rm\,s}\xspace}$, we see the bolometric flux holding constant, causing an excess over the cooling trend that coincides exactly with the second peak observed in the light curve. Hence, the spectroscopy 