  A recent report has identified a central compact object (CCO) within the
supernova remnant HESS J1731-347, with a mass and radius of
$M=0.77^{+0.20}_{-0.17}M{\odot}$ and $R=10.4^{+0.86}_{-0.78}$ km, respectively.
To investigate this light compact star, a density-dependent relativistic
mean-field (DDRMF) model, specifically the DDVT model, has been employed. The
DDVT model incorporates tensor couplings of vector mesons, which {can}
successfully describe the properties of finite nuclei, such as charge radius,
binding energy, and spin-orbit splitting. The introduction of tensor coupling
reduces the influence of scalar mesons and generates a softer equation of state
(EOS) in the outer core of the neutron star. Moreover, it has been found that
the crust segment plays a crucial role in reproducing the mass-radius relation
of HESS J1731-347, indicating a preference for a soft crust EOS. By
manipulating the coupling strength of the isovector meson in the DDVT parameter
set, a reasonable hadronic EOS has been obtained, satisfying the constraints
from the gravitational-wave signal GW170817, the simultaneous mass-radius
measurements from the NICER collaboration, and the properties of finite nuclei.
Notably, the mass-radius relations derived from this hadronic EOS also
accurately describe the observables of HESS J1731-347. Therefore, based on our
estimation, the CCO in HESS J1731-347 may represent the lightest known neutron
star.
