In a recent work, we applied a QCD-based EOS 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. We have also compared our results with the most recent astrophysical 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 compatible with all astrophysical observations but the parameter window is now narrower. We observe a tension between the radius and the tidal deformability of the star. In this contribution, we expand the discussion of the results found in our previous paper.