  The ultra-short-period (USP) planets are exoplanets with very short orbital
periods ($\textit{P} < 1$ day), and TOI-1807b is one such planet recently
discovered by the TESS mission where it orbits in the TOI-1807 system that is
still little known nowadays. In this paper, we re-analyzed the transit light
curves of TOI-1807 using the latest TESS data from Sector 49, combined with
previous data from Sector 22 and 23. By running the MCMC simulation through all
three sectors, we found that our transit model fits the data from Sector 49 the
best, and we deduced that TOI-1807b is a Super-Earth with a mass of
$2.27^{+0.49}_{-0.58}\, M_\oplus$, a radius of $1.37^{+0.10}_{-0.09}\,
R_\oplus$, a density of $0.875^{+0.264}_{-0.285}\, \rho_\oplus$, and a surface
temperature of $1499^{+82}_{-129}\, \mathrm{K}$. We confirmed that TOI-1807b
orbits at approximately $0.0135^{+0.0013}_{-0.0022}\, \mathrm{AU}$ with a
period of $0.54929^{+0.00012}_{-0.00005}\, \mathrm{days}$, which raises the
possibility of the planet being tidally locked due to spin-orbit
synchronization. In addition, we suggest that TOI-1807b might slowly undergo
its orbital decay process, and we further identify that TOI-1807b is in a
circular, synchronous orbit and permanently deformed due to tides, leading to
$\sim$4% correction in density. Since TOI-1807 is such a young star with an age
of only $300 \pm 80\, \mathrm{Myr}$, we also imply that the radiation emitted
from active TOI-1807 could be so intense that it might have destroyed most of
the atmosphere over the surface of TOI-1807b.
