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I will present a calculation of the perturbative QCD corrections to the equation of state (EoS) of neutron stars, which involves the computation of Feynman loop integrals with a non-zero chemical potential. Modern tools used in the calculation of loop corrections in collider physics, for which the chemical potential vanishes, can be adapted to streamline the calculation of the integrals required to constrain the EoS of neutron stars at large energy densities. I will describe these tools, how they can be employed in this context, and argue that they are mature enough to allow us to extend the current state of the art in the near future.