Hybrid Stars that Masquerade as Neutron Stars

By M. Alford, Matt Braby, Mark Wayne Paris, S. Reddy. 2004

584 citations recorded by the source corpus.

We show that a hybrid (nuclear+quark matter) star can have a mass-radius relationship very similar to that predicted for a star made of purely nucleonic matter. We show this for a generic parameterization of the quark matter equation of state and also for an MIT bag model, each including a phenomenological correction based on gluonic corrections to the equation of state. We obtain hybrid stars as heavy as 2 M☉ for reasonable values of the bag model parameters. For nuclear matter, we use the equation of state calculated by Akmal and coworkers using many-body techniques. Both mixed and homogeneous phases of nuclear and quark matter are considered.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7b2ff50e008c27accc36e07d1ca5de7290f1e493

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Citations in the corpus

Generic conditions for stable hybrid stars (2013, background): “, [11, 22], which found that in the absence of theoretical or experimental constraints on the quark matter EoS, one can fairly easily vary the unknown parameters of that EoS to obtain heavy hybrid stars.”
From hadrons to quarks in neutron stars: a review (2017, background): “The similarity of radii in hybrid and pure nuclear matter stars is analyzed in [231].”
Composition and stability of hybrid stars with hyperons and quark color-superconductivity (2011, methodology): “…the quark matter equation of state motivated by the MIT bag model in combination with nuclear equations of state that are moderately soft; large masses require strong quark-quark correlations in combinatio with color superconductivity in the CFL phase (Alford et al. 2005; Weissenborn et al. 2011).”
A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars (2014, background): “The last case has been dubbed the “masquerade” problem Alford et al. (2005).”
INTERACTING QUARK MATTER EQUATION OF STATE FOR COMPACT STARS (2013, methodology): “Finally, it should be noted that during the past 15 yr there have been several attempts to describe various perturbative EOSs with fitting functions of increasing sophistication (see, e.g., Fraga et al. 2001; Alford et al. 2005).”
CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, background): “2(a), for pure quark matter the larger bag constant gives a lower total pressure, while the inclusion of first order αs corrections stiffens the quark EoS (see also Alford et al. 2005).”
Maximum mass of neutron stars and strange neutron-star cores (2012, methodology): “1, including of a mixed-phase state does not change, to a very good approximation, the value of Mmax (Alford et al. 2005).”
Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, background): “Whether quark matter (QM) exists and how big its mass or volume may be are among the longstanding and interesting issues regarding the structure of neutron stars [109].”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “Moreover, along the decades other stellar objects have appeared in the literature, such as hyperon stars [11], quark/hybrid stars [12, 13], strange stars [14], and even more exotic objects such as boson stars [15].”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “normal matter in the form of neutrons, protons, electrons, and muons, or kaon condensates [117, 118], hyperons [119–121], and quark-gluon plasmas [46]) or even pure quark matter [47].”