Hadron-quark phase transition in dense matter and neutron stars

By G. Fiorella Burgio, Marc A. Baldo, Hans-Josef Schulze, Pradip Kumar Sahu. 2002

141 citations recorded by the source corpus.

We study the hadron-quark phase transition in the interior of neutron stars (NS's). We calculate the equation of state (EOS) of hadronic matter using the Brueckner-Bethe-Goldstone formalism with realistic two-body and three-body forces, as well as a relativistic mean field model. For quark matter we employ the MIT bag model constraining the bag constant by using the indications coming from the recent experimental results obtained at the CERN SPS on the formation of a quark-gluon plasma. We find it necessary to introduce a density-dependent bag parameter and the corresponding consistent thermodynamical formalism. We calculate the structure of NS interiors with the EOS comprising both phases, and we find that the NS maximum masses fall in a relatively narrow interval, $1.4{M}_{\ensuremath{\bigodot}}l~{M}_{\mathrm{max}}l~{1.7M}_{\ensuremath{\bigodot}}.$ The precise value of the maximum mass turns out to be only weakly correlated with the value of the energy density at the assumed transition point in nearly symmetric nuclear matter.

Subfields: Astronomy and Astrophysics, Geophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b3b309121e356558492e988edfd6dcca0430cdfa

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. Matt Braby
2. Mark Wayne Paris
3. S. Reddy
4. M. Alford
5. Armen Sedrakian
6. P. Haensel
7. J. Zdunik
8. L. Bonanno

In Geophysics

1. Matt Braby
2. Mark Wayne Paris
3. S. Reddy
4. M. Alford

In Nuclear and High Energy Physics

1. S. Reddy
2. M. Alford
3. P. Haensel
4. Armen Sedrakian
5. J. Zdunik
6. L. Bonanno
7. E. O’Connor

Citations in the corpus

• Unified equation of state for neutron stars on a microscopic basis (2015, unknown): “Many models for the deconfined quark matter produce a too soft EoS to support a NS of mass compatible with observations (Burgio et al. 2002a,b; Baldo et al. 2003, 2008a; Maieron et al. 2004; Nicotra et al. 2006; Chen et al. 2011).”
• Hybrid Stars that Masquerade as Neutron Stars (2004, methodology): “…stars are predicted to have lower maximum mass (M P 1:7 M ) than nuclear matter stars (M P 2:2 M ) (Lattimer & Prakash 2001; Haensel 2003;Maieron et al. 2004; Alford & Reddy 2003; Buballa et al. 2004; Banik &Bandyopadhyay 2003; Burgio et al. 2002a, 2002b; Gocke et al. 2001; Schertler et al. 2000).”