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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Maximum M<strong>as</strong>ses <strong>of</strong> Neutron Stars – Causality<br />
3.5<br />
3<br />
RMF TM1<br />
n crit =2.5 n 0<br />
n crit =2 n 0<br />
n crit =3 n 0<br />
2.5<br />
M [M solar ]<br />
2<br />
1.5<br />
1<br />
0.5<br />
9 10 11 12 13 14 15 16<br />
R [km]<br />
(Sagert, Sturm, Chatterjee, Tolos, JSB in preparation)<br />
RMF parameter set TM1: fitted to properties <strong>of</strong> spherical nuclei<br />
above a fiducial density (determined from <strong>the</strong> analysis <strong>of</strong> <strong>the</strong> KaoS heavy-ion<br />
data) transition to stiffest possible EoS<br />
causality argument: p = ǫ−ǫ c above <strong>the</strong> fiducial density ǫ f<br />
Rhoades, Ruffini (1974), Kalogera, Baym (1996): M max = 4.2M ⊙ (ǫ 0 /ǫ f ) 1/2<br />
=⇒ new upper m<strong>as</strong>s limit <strong>of</strong> about 2.8M ⊙ from heavy-ion data!<br />
– p.18
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