  Context: Recently, Doroshenko and collaborators reported a very low-mass
compact star, a Central Compact Object named XMMU J173203.3-344518 inside the
supernova remnant HESS J1731-347. Its tiny mass is at odds with all
calculations of minimum masses of neutron stars generated by iron cores,
therefore (and even if not compellingly) it has been suggested to be a {\it
strange star}. Besides the mass, a radius and surface temperature have been
extracted from data, and the whole body of information should ultimately reveal
if this object is truly consistent with an exotic composition.
  Aims: To understand the status of the compact object XMMU J173203.3-344518 in
HESS J1731-347 within the existing models of strange stars, including its
prompt formation.
  Methods: The information obtained on the mass, radius and surface temperature
are compared to theoretical calculations performed within usual theoretical
models using General Relativity as the assumed theory of gravitation and a
handful of cooling scenarios. A qualitative discussion showing the consistency
of the strange-matter driven supernova scenario with a low-mass compact star is
provided.
  Results: We found that the object HESS J1731-347 fits within the same quark
star models recently employed to explain the masses and radii of the NICER
objects PSR J040+6620 and PSR J0030+0451, in which both quantities were
simultaneously determined. It is also remarkable to find that a simple cooling
scenario devised $30\text{ yr}$ ago with superconducting quarks provides an
overall good explanation of the surface temperature.
  Conclusions: We conclude that XMMU J173203.3-344518 in the remnant HESS
J1731-347 fits into a ``strange star'' scenario that is also consistent with
heavier compact stars, which can also belong to the same class and constitute
an homogeneous type of self-bound objects produced in Nature.
