Strange quark matter in explosive astrophysical systems
Explosive astrophysical systems, such as supernovae or compact star binary mergers, provide conditions where strange quark matter can appear. The high degree of isospin asymmetry and temperatures of several MeV in such systems may cause a transition to the quark phase already around saturation densi...
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| Hauptverfasser: | , , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
12 August 2010
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| In: |
Journal of physics. G, Nuclear and particle physics
Year: 2010, Jahrgang: 37, Heft: 9, Pages: 1-6 |
| ISSN: | 1361-6471 |
| DOI: | 10.1088/0954-3899/37/9/094064 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1088/0954-3899/37/9/094064 Verlag, lizenzpflichtig, Volltext: https://dx.doi.org/10.1088/0954-3899/37/9/094064 
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| Verfasserangaben: | Irina Sagert, T Fischer, M Hempel, G Pagliara, J Schaffner-Bielich, F-K Thielemann and M Liebendörfer |
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| 520 | |a Explosive astrophysical systems, such as supernovae or compact star binary mergers, provide conditions where strange quark matter can appear. The high degree of isospin asymmetry and temperatures of several MeV in such systems may cause a transition to the quark phase already around saturation density. Observable signals from the appearance of quark matter can be predicted and studied in astrophysical simulations. As input in such simulations, an equation of state with an integrated quark matter phase transition for a large temperature, density and proton fraction range is required. Additionally, restrictions from heavy ion data and pulsar observation must be considered. In this work we present such an approach. We implement a quark matter phase transition in a hadronic equation of state widely used for astrophysical simulations and discuss its compatibility with heavy ion collisions and pulsar data. Furthermore, we review the recently studied implications of the QCD phase transition during the early post-bounce evolution of core-collapse supernovae and introduce the effects from strong interactions to increase the maximum mass of hybrid stars. In the MIT bag model, together with the strange quark mass and the bag constant, the strong coupling constant αs provides a parameter to set the beginning and extension of the quark phase and with this the mass and radius of hybrid stars. | ||
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