The Structure of the Hadron-Quark Combustion Zone

Abstract

Hadron-quark combustion in dense matter is a central topic in the study of phases in compact stars and their high-energy astrophysics. We critically review the literature on hadron-quark combustion, dividing them into a "first wave" that treats the problem as a steady-state burning with or without constraints of mechanical equilibrium, and a "second wave" which uses numerical techniques to resolve the burning front and solves the underlying Partial Differential Equations for the chemistry of the burning front under less restrictive conditions. We detail the inaccuracies that the second wave amends over the first wave, and highlight crucial differences between various approaches in the second wave. We also include results from time-dependent simulations of the reaction zone that include a hadronic EOS, neutrinos, and self-consistent thermodynamics without using parameterized shortcuts.

The Macro-Physics of the Quark-Nova: Astrophysical Implications

“…Ultimately, it is the transport of s-quarks, in concert with neutrino transport and leptonic dynamics, that decides the behavior of the flame, which is very different from the way thermal conductivity acts in Arrhenius-type reactions. Thus, fundamentally, the non-premised scenario in the quark-nova model is different from that of past work (see in-depth analysis and discussion in [35,36]).…”

A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

“…While such a transition is already hinted at by analytical (e.g. Keränen et al 2005;Vogt et al 2004;) and by one-dimensional numerical simulations (Niebergal et al 2010;Ouyed, A. et al 2018a,b; see also Ouyed, A. et al 2019), detailed multi-dimensional simulations are required to prove or disprove our working hypothesis (Niebergal 2011;Ouyed, A. 2018).…”

“…Besides the limitations listed in Section 8.4, our model relies on the feasibility of a delayed explosive transition of a massive NS to a QS years to decades following the SN explosion of a massive star. While such a transition is already hinted at by analytical (e.g., Keränen et al 2005;Vogt et al 2004; and by onedimensional numerical simulations (Niebergal et al 2010;Ouyed et al 2018b,a; see also Ouyed et al 2019), detailed multi-dimensional simulations are required to verify or refute our working hypothesis (Niebergal 2011;Ouyed 2018). Furthermore, a full treatment of the interaction between the relativistic QN ejecta and the turbulent and non-turbulent PWN-SN shell would require detailed hydrodynamical simulations beyond the scope of this paper.…”

“…The neutrino burst during the first few milliseconds that follow a QN is about two orders of magnitude brighter than the SN signal since the neutrino-sphere of a proto-QS is much hotter than in the proto-NS case (see Ouyed, A. (2018); Ouyed, A. et al (2019)). Neutrino observatories, such as Super-Kamiokande-III (Ikeda et al 2007) should in principle distinguish between the SN and QN neutrino signals.…”

“…Thus during the first few milliseconds that follow a QN, the neutrino signal is harder and brighter (by a factor of about (20/5) 4 ∼ 200) than the SN one. This translates to a peak detector count for QNe that is about a thousand times higher than the peak detector count for SNe (see Ouyed (2018); Ouyed et al (2019)). Neutrino observatories, such as Super-Kamiokande-III (Ikeda et al 2007) should in principle distinguish between the SN and QN neutrino signals.…”