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Description
A first order phase transition to quark matter can provide a shock revival mechanism for core-collapse supernovae and a means to enhance the energy of the explosion. Recent studies have also noted the onset of radial oscillations of the core that can be excited when the equation of state allows the formation quark matter. Such oscillations may produce an observable signal in emitted neutrinos. In this work, expand on previous models in spherical symmetry by including effects neutrino-heated convection based upon Supernovae Turbulence in Reduced-Dimensionality (STIR). We analyze a set of solar-metallicity progenitor models from 14 - 40 $M_{\odot}$ in. We find that most models with turbulence tend to explode before reaching the secondary shock or oscillations from the phase transition. This implies that it may be difficult to observe the oscillations. Nevertheless, at least two models experience the onset of oscillations. We also analyze the source of the oscillations and show that they result when the quark matter coexistence region realizes an equation of state with an adiabatic index of 4/3. This occurs relatively far out in the star. The resulting oscillations are not a pure breathing mode, but have a node at the radius where the adiabatic index crosses 4/3. We present semi-analytic models for the onset and frequency of the oscillations.
| Category | Theory |
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