Cold quark matter

By A. Kurkela, Paul Romatschke, A. Vuorinen. 2009

328 citations recorded by the source corpus.

We perform an O({alpha}{sub s}{sup 2}) perturbative calculation of the equation of state of cold but dense QCD matter with two massless and one massive quark flavor, finding that perturbation theory converges reasonably well for quark chemical potentials above 1 GeV. Using a running coupling constant and strange quark mass, and allowing for further nonperturbative effects, our results point to a narrow range where absolutely stable strange quark matter may exist. Absent stable strange quark matter, our findings suggest that quark matter in (slowly rotating) compact star cores becomes confined to hadrons only slightly above the density of atomic nuclei. Finally, we show that equations of state including quark matter lead to hybrid star masses up to M{approx}2M{sub {center_dot},} in agreement with current observations. For strange stars, we find maximal masses of M{approx}2.75M{sub {center_dot}}and conclude that confirmed observations of compact stars with M>2M{sub {center_dot}}would strongly favor the existence of stable strange quark matter.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3006ce5d82cb64a3219fcfa8b9f1a6ada5863856

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. I. Tews
2. S. Reddy
3. M. Hempel
4. A. Kurkela
5. A. Vuorinen
6. Stefano Gandolfi
7. J. Carlson
8. Tobias Fischer

In Nuclear and High Energy Physics

1. I. Tews
2. S. Reddy
3. M. Hempel
4. A. Kurkela
5. A. Vuorinen
6. Stefano Gandolfi
7. J. Carlson
8. E. Fraga

Citations in the corpus

• QUARK MATTER IN MASSIVE COMPACT STARS (2011, background): “…that effects from the strong interaction, such as one-gluon exchange or colorsuperconductivity can stiffen the quark matter EoS and increase the maximum mass of quark and hybrid stars (Rüster & Rischke 2004; Horvath & Lugones 2004; Alford et al. 2007; Fischer et al. 2010; Kurkela et al. 2010a,b).”
• INTERACTING QUARK MATTER EQUATION OF STATE FOR COMPACT STARS (2013, methodology): “The calculation relevant for compact star physics is clearly theO(α2s ) zero-temperature work of Kurkela et al. (2010a), which most importantly also takes into account the non-zero value of the strange quark mass.”
• Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations (2018, methodology): “In the following, we shall connect the speed of sound in neutron matter at densities up to 1−2n0 shown in Figure 3, to the speed of sound expected in deconfined quark matter at very high density(Kurkela et al. 2010) using two parameterizations, that we will discuss in Sections 3.1 and 3.2.”
• Inverse magnetic catalysis in dense holographic matter (2010, unknown): “[68, 69]).”
• Symmetry energy impact in simulations of core-collapse supernovae (2013, background): “n-hyperon interactions or many-body forces including hyperons [37,38,39,40]. For quark matter, strong QCD interactions have been shown to provide sucient pressure to support high neutron star masses [41,42,43, 44,45,46,47]. From the current understanding of strong interactions, neither hyperon nor q”