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The recent detection of gravitational waves from merging neutron star eventshas opened a new window on the many unknown aspects of their internal dynamics.A key role in this context is played by the transition from baryon to quarkmatter described in the neutron star equation of state (EoS). In particular,the binary pulsar observation of heavy neutron stars requires appropriatelystiff dense matter in order to counter gravitational collapse, at variance withthe predictions of many phenomenological quark models. On the other side, theLIGO observations favor a softer EoS therefore providing a lower bound to theequation stiffness. We introduce a quantum chromodynamics (QCD) description ofthe neutron star's high baryon density regime where the pressure and energydensity distributions are directly obtained from the matrix elements of the QCDenergy momentum tensor. Recent ab initio calculations allow us to evaluate theenergy-momentum tensor in a model independent way including both quark andgluon degrees of freedom. Our approach is a first effort to replace quarkmodels and effective gluon interactions with a first principles, fullyQCD-based description. Most importantly, the QCD energy momentum tensor matrixelements are connected to the Mellin moments of the generalized partondistributions which can be measured in deeply virtual exclusive scatteringexperiments. As a consequence, we establish a connection between observablesfrom high energy experiments and from the analysis of gravitational waveevents. Both can be used to mutually constrain the respective sets of data. Inparticular, the emerging QCD-based picture is consistent with the GW170817neutron star merger event once we allow a first-order phase transition from alow-density nuclear matter EoS to the newly-constructed high-densityquark-gluon one.

Bounds on the Equation of State of Neutron Stars from High Energy Deeply Virtual Exclusive Experiments