Generic conditions for stable hybrid stars
By M. Alford, Sophia Han, M. Prakash. 2013
261 citations recorded by the source corpus.
We study the mass-radius curve of hybrid stars, assuming a single first-order phase transition between nuclear and quark matter, with a sharp interface between the quark matter core and nuclear matter mantle. We use a generic parameterization of the quark matter equation of state, which has a constant, i.e. density-independent, speed of sound ("CSS"). We argue that this parameterization provides a framework for comparison and empirical testing of models of quark matter. We obtain the phase diagram of possible forms of the hybrid star mass-radius relation, where the control parameters are the transition pressure, energy density discontinuity, and the quark matter speed of sound. We find that this diagram is sensitive to the quark matter parameters but fairly insensitive to details of the nuclear matter equation of state. We calculate the maximum hybrid star mass as a function of the parameters of the quark matter EoS, and find that there are reasonable values of those parameters that give rise to hybrid stars with mass above $2\,M_\odot$.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/e70434d4a2f26ce32da4915479986473868a385d
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In Astronomy and Astrophysics
Citations in the corpus
- From hadrons to quarks in neutron stars: a review (2017, background): “see figure 18 of [52]); [254] summarizes qualitatively possible conditions on the quark matter equation of state that would support neutron stars of two solar masses.”
- A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars (2014, methodology): “…2013; Alford et al. 2013): (1) The latent heat of the phase transition should fulfil a constraint Δε > Δεmin (Haensel et al. 2007; Zdunik & Haensel 2013; Alford et al. 2013), where Δεmin ∼ 0.6εcrit for the schematic hybrid EoS investigated in Alford et al. (2013) and Alvarez-Castillo & Blaschke…”
- CONSTRAINING THE SYMMETRY PARAMETERS OF THE NUCLEAR INTERACTION (2012, background): “Alford et al. (2013) also explored the effects of phase transitions in hybrid stars, but also included the dependence on L in their study.”
- New Neutron Star Equation of State with Quark–Hadron Crossover (2019, background): “…conventional description of the transition from hadronic matter to weakly interacting quark matter via a first order transition (Baym & Chin (1976); Alford et al. (2013)), the transition occurs gradually in the range 2-5 n0 without a discontinuous jump (or perhaps with a small jump) in the energy…”
- Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, methodology): “It was connected through the Maxwell construction to the Constant Speed of Sound (CSS) model for quark matter developed by Alford, Han, and Prakash [123].”
- Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations (2018, background): “…2n0, and models of highdensity matter where new Fermionic or bosonic degrees of freedom appear suddenly to produce discontinuities in the energy density (note that the pressure is continuous and monotonically increasing toward the center of NS due to hydrostatic equilibrium; Alford et al. 2013).”
- Unified equation of state for neutron stars on a microscopic basis (2015, background): “The quark-quark interaction in the deconfined phase must be more repulsive in order to stiffen the EoS, and indeed, with a suitable quark-quark interaction, mixed quark-nucleon matter can have an EoS compatible with two solar masses or more (Alford et al. 2013).”