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The recent analysis on the central compact object in the HESS J1731-347remnant suggests interestingly small values for its mass and radius. Such anobservation favors soft nuclear models that may be challenged by theobservation of massive compact stars. In contrast, the recent PREX-IIexperiment, concerning the neutron skin thickness of $^{208}$Pb, points towardsstiff equations of state that favor larger compact star radii. In the presentstudy, we aim to explore the compatibility between stiff hadronic equations ofstate (favored by PREX-II) and the HESS J1731-347 remnant in the context ofhybrid stars. For the construction of hybrid equations of state we use threewidely employed Skyrme models combined with the well-known vector MIT bagmodel. Furthermore we consider two different scenarios concerning the energydensity of the bag. In the first case, that of a constant bag parameter, wefind that the resulting hybrid equations of state are strongly disfavored bythe observation of $\sim2 M_\odot$ pulsars. However, the introduction of aGaussian density dependence yields results that are compatible with theconservative $2 M_\odot$ constraint. The utilization of recent data based onthe observation of PSR J0030+0451, PSR J0952-0607 and GW190814 allows for theimposition of additional constraints on the relevant parameters and thestiffness of the two phases. Interestingly, we find that the derived hybridequations of state do not satisfy the PSR J0030+0451 constraints in $1\sigma$and only marginally agree with the $2\sigma$ estimations. In addition, weestimate that the observation of massive pulsars, like PSR~J0952-0607, incombination with the existence of HESS J1731-347, may require a strong phasetransition below $\sim 1.7n_0$. Finally, we show that the supermassive compactobject involved in GW190814 could potentially be explained as a rapidlyrotating hybrid star.

Hybrid stars in light of the HESS J1731-347 remnant and the PREX-II experiment