QCD in the cores of neutron stars
Oleg Komoltsev
TL;DR
This paper explores how advanced perturbative QCD calculations at high densities inform the equation of state for neutron star cores, providing theoretical constraints that complement astrophysical data.
Contribution
It demonstrates that high-density QCD calculations can constrain neutron star matter properties at lower densities, bridging theoretical physics and astrophysical observations.
Findings
Perturbative QCD at high densities constrains neutron star EOS.
Theoretical calculations complement astrophysical data.
QCD insights inform neutron star matter understanding.
Abstract
I discuss why state-of-the art perturbative QCD calculations of the equation of state at large chemical potential that are reliable at asymptotically high densities constrain the same equation of state at neutron-star densities. I describe how these theoretical calculations affect the EOS at lower density. I argue that the ab-initio calculations in QCD offer significant information about the equation of state of the neutron-star matter, which is complementary to the current astrophysical observations.
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Taxonomy
TopicsPulsars and Gravitational Waves Research · Atomic and Subatomic Physics Research · Gamma-ray bursts and supernovae