  In an early work, we applied a QCD-based equation of state to the study of
the stellar structure of self-bound strange stars, obtaining sequences with
maximum masses larger than two solar masses and radii ranging from 8 to 12 Km.
In this work, we update the previous calculations and compare them with the
most recent data, including the very recent determination of the mass and
radius of the massive pulsar PSR J0740+6620 performed by the NICER and
XMM-Newton Collaborations. Our equation of state is similar to the MIT bag
model one, but it includes repulsive interactions, which turn out to be
essential to reproduce the accumulated experimental information. We find that
our EOS is still compatible with all astrophysical observations but the
parameter window is now narrower.
