# Evidence for quark-matter cores in massive neutron stars

**Authors:** Eemeli Annala, Tyler Gorda, Aleksi Kurkela, Joonas N\"attil\"a, Aleksi, Vuorinen

arXiv: 1903.09121 · 2021-07-28

## TL;DR

This paper provides evidence that the cores of the most massive neutron stars likely contain deconfined quark matter, based on combining astrophysical data with theoretical calculations, impacting neutron star physics and merger dynamics.

## Contribution

It offers the first model-independent evidence for quark-matter cores in massive neutron stars by integrating observations with ab-initio calculations.

## Key findings

- Massive neutron stars likely have quark-matter cores.
- Presence of quark matter depends on the speed of sound in dense matter.
- Implications for neutron star phenomenology and merger behavior.

## Abstract

The theory governing the strong nuclear force, Quantum Chromodynamics, predicts that at sufficiently high energy densities hadronic nuclear matter undergoes a deconfinement transition to a new phase of quarks and gluons. Although this has been observed in ultrarelativistic heavy-ion collisions, it is currently an open question whether quark matter exists inside neutron stars. By combining astrophysical observations and theoretical ab-initio calculations in a model-independent way, we find that the inferred properties of matter in the cores of neutron stars with mass corresponding to 1.4 solar masses are compatible with nuclear model calculations. However, the matter in the interior of maximally massive, stable neutron stars exhibits characteristics of the deconfined phase, which we interpret as evidence for the presence of quark-matter cores. For the heaviest reliably observed neutron stars with masses of about two solar masses, the presence of quark matter is found to be linked to the behaviour of the speed of sound c_s in strongly interacting matter. If the conformal bound (c_s)^2 < 1/3 is not strongly violated, massive neutron stars are predicted to have sizable quark-matter cores. This finding has important implications for the phenomenology of neutron stars, and affects the dynamics of neutron star mergers with at least one sufficiently massive participant.

## Full text

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## Figures

8 figures with captions in the complete paper: https://tomesphere.com/paper/1903.09121/full.md

## References

49 references — full list in the complete paper: https://tomesphere.com/paper/1903.09121/full.md

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Source: https://tomesphere.com/paper/1903.09121