neutron stars - Universität Heidelberg

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QCD phase transition in supernovae Irina Sagert, Matthias Hempel, Giuseppe Pagliara, JSB, Tobias Fischer, Anthony Mezzacappa, Friedel Thielemann, Matthias Liebendörfer, arXive:0809.4225, submitted to PRL – p.30
Phase Transition to Quark Matter for Astros T [MeV] 100 90 80 70 60 50 40 30 20 10 B 1/4 =165 MeV, m s =100 MeV, m u =m d =0 0 0 0.05 0.1 0.15 0.2 0.25 0.3 0.35 0.4 0.45 nb [fm -3 ] Y p =0.5 Y p =0.3 Y p =0.05 (Irina Sagert and Giuseppe Pagliara) quark matter appears at low density due to β-equilibrium low critical density for low Yp due to nuclear asymmetry energy quark matter favoured at finite temperature supernova matter at bounce: T = 20 − 30 MeV, Yp = 0.2 − 0.3, ǫ ∼ (1 − 1.5)ǫ0 – p.31
Page 1 and 2: Neutron Stars, Quark Stars and the
Page 3 and 4: UniSpiegel, Universität Heidelberg
Page 5 and 6: Rhein-Neckar-Zeitung, 09.01.2009 my
Page 7 and 8: Observational Data on Neutron Stars
Page 9 and 10: Neutron Stars Movie (seven still im
Page 11 and 12: Masses of Pulsars (Stairs, 2006) mo
Page 13 and 14: How To Measure Masses AND Radii of
Page 15 and 16: Constraints on the Mass-Radius Rela
Page 17 and 18: Neutron Star versus Strange Quark S
Page 19 and 20: X-Ray burster binary systems of a n
Page 21 and 22: Properties of Neutron Stars and Qua
Page 23 and 24: Structure of a Neutron Star — the
Page 25 and 26: Quark matter in the NJL model p = 1
Page 27 and 28: Mass-radius and maximum density of
Page 29 and 30: Quark star twins? (Fraga, JSB, Pisa
Page 31: Signals for the QCD Phase Transitio
Page 35 and 36: Check: Mass-Radius Diagram of Cold
Page 37 and 38: Implications for Supernovae - Explo
Page 39 and 40: Implications for Supernovae - Explo
Page 41 and 42: Summary quark matter can be present

neutron stars - Universität Heidelberg

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