Numerical Simulation of the Hydrodynamical Combustion to Strange Quark Matter

Abstract

We present results from a numerical solution to the burning of neutron matter inside a cold neutron star into stable (u,d,s) quark matter. Our method solves hydrodynamical flow equations in 1D with neutrino emission from weak equilibrating reactions, and strange quark diffusion across the burning front. We also include entropy change due to heat released in forming the stable quark phase. Our numerical results suggest burning front laminar speeds of 0.002-0.04 times the speed of light, much faster than previous estimates derived using only a reactive-diffusive description. Analytic solutions to hydrodynamical jump conditions with a temperature dependent equation of state agree very well with our numerical findings for fluid velocities. The most important effect of neutrino cooling is that the conversion front stalls at lower density (below approximately 2 times saturation density). In a 2-dimensional setting, such rapid speeds and neutrino cooling may allow for a flame wrinkle instability to develop, possibly leading to detonation.

5 pages, 3 figures (animations online at http://www.capca.ucalgary.ca/~bniebergal/webPHP/research.php)

References in corpus (8)

• Signals of the QCD phase transition in core-collapse supernovae
• Mass Ejection by Strange Star Mergers and Observational Implications
• Type Ia Supernova: Calculations of Turbulent Flames Using the Linear Eddy Model
• Supernova SN2006gy as a first ever Quark Nova?
• Nucleosynthesis in neutron-rich ejecta from quark-novae
• The effect of turbulent intermittency on the deflagration to detonation transition in SN Ia explosions
• Formation of Quark Phases in compact stars and their connection to Gamma-Ray-Bursts
• New Approaches for Modeling Type Ia Supernovae

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