Pulsars as a probe for the nuclear and quark matter equation of state
Pulsars as a probe for the nuclear and quark matter equation of state
Pulsars as a probe for the nuclear and quark matter equation of state
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Hybrid Stars with a stiff <strong>nuclear</strong> EoS<br />
– p.14<br />
2.8<br />
2.6<br />
a 4 =0.4<br />
Maximum M<strong>as</strong>s [M solar ]<br />
2.4<br />
2.2<br />
2<br />
1.8<br />
1.6<br />
1.4<br />
a 4 =0.5<br />
120 140 160 180 200 220 240 260 280 300<br />
B eff<br />
1/4 [MeV]<br />
a 4 =1.0<br />
PSR J1614-2230<br />
Maxwell hybrid stars<br />
1.67 M<br />
Maxwell, <strong>quark</strong> core<br />
solar<br />
Gibbs, <strong>quark</strong> core<br />
Gibbs, mixed core<br />
n c ~ 0.1 1/fm 3<br />
1.44 M<br />
n c ~ 0.2 1/fm 3<br />
solar n c ~ 0.3 1/fm 3<br />
n c ~ 0.4 1/fm 3<br />
n c ~ 0.5 1/fm 3<br />
(Weissenborn, Sagert, Pagliara, Hempel, JSB 2011)<br />
<strong>nuclear</strong> ph<strong>as</strong>e: relativistic mean field model with parameter set NL3 (fitted to<br />
properties <strong>of</strong> nuclei)<br />
match with Gibbs (lines) or Maxwell construction (shaded area)<br />
solid lines: pure <strong>quark</strong> <strong>matter</strong> cores, d<strong>as</strong>hed lines: mixed ph<strong>as</strong>e cores
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