Thomas Klähn D. Blaschke R. Łastowiecki F. Sandin 20.5.2011Thomas Klähn – Three Days on...

Thomas KlähnD. BlaschkeR. ŁastowieckiF. Sandin

20.5.2011Thomas Klähn – Three Days on Quarkyonic Island

COMPACT STARS, HEAVY ION COLLISIONS AND LESSONS FOR QCD

Thomas Klähn – Three Days on Quarkyonic Island

CONCLUSION

20.5.2011

of the “CompStar School and Workshop” (Catania - May 3-12, 2011)

The most exciting news of the last year:

• Mass of Pulsar J1614-2230 : Demorest et al., Nature 467, 1081-1083 (2010)• Rapid cooling of Cas A Heinke, Ho, Astrophys. J. Lett., 719, L167 (2010)

sunM)04.097.1(M

Page, Prakash, Lattimer, Steiner, Phys.Rev.Lett.106:081101 (2011)Blaschke, Grigorian, Prog.Part.Nucl.Phys. 59 (2007)


CONCLUSION

20.5.2011

of the “CompStar School and Workshop” (Catania - May 3-12, 2011)

The most exciting news of the last year are:

• Mass of Pulsar J1614-2230 : P.Demorest et al., Nature 467, 1081-1083 (2010)

What are the consequences for the existence of quark matter in Compact Stars?

sunM)04.097.1(M


PSR J1614-2230

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Binary system in Scorpius ہparsecs from Earth 1200 ہNeutron star with white dwarf companion ہNS - millisecond pulsar (P=3.15 ms) ہ

.Time signal is getting delayed when passing near massive object ہ.General relativistic effect ہ.Size of the effect depends on the mass and inclination angle ہPulse delay best to measure when pulsar is exactly behind companion ہ


PSR J1614-2230

20.5.2011

Binary system in Scorpius ہparsecs from Earth 1200 ہNeutron star with white dwarf companion ہNS - millisecond pulsar (P=3.15 ms) ہRecycled pulsar – accretion ہ

.Time signal is getting delayed when passing near massive object ہ.General relativistic effect ہ.Size of the effect depends on mass and inclination angle ہPulse delay best to measure when pulsar is exactly behind companion ہ


PSR J1614-2230

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Observational Results:

inclination angle 89.17 ہ

.companion mass of 0.5 solar masses ہcompanion is a helium-carbon-oxygen white dwarf ہ


PSR J1614-2230

20.5.2011

Observational Results:

inclination angle 89.17 ہ

.companion mass of 0.5 solar masses ہcompanion is a helium-carbon-oxygen white dwarf ہ

:neutron star mass ہ

WORLD (universal? intergalactic?) RECORD! P.Demorest et al., Nature 467, 1081-1083 (2010)

:Highest well known mass of NS before ہ

sunM)04.097.1(M

sunM66.1


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Nuclear matter far beyond saturation density is not well understood:

Klähn et al., Phys.Rev. C74 (2006) 035802

WHY PSR J1614 IS SO EXCITING



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Large neutron star masses (about and more) provide a serious constraint.Sun2MKlähn et al., Phys.Rev. C74 (2006) 035802



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Klähn et al., Phys.Rev. C74 (2006) 035802



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INTERESTING!!!

If UB confirmed unambiguously...

HIC can constrain maximum NS mass!

... which we estimated quite a time ago:

sunmax M1.20.2M Klähn et al., Phys.Rev. C74 (2006) 035802


PSR J1614 AND QUARK MATTER

20.5.2011

Can QM be present in PSR J1614?

Presently, one cannot knowwhether quark matter exists in PSR J1614.

However, if there is NOquark matter in this object,it is in no other NS we know.

Why is this so?

The more massive a NS isthe higher is the central density.

Would clarifying the question of QM in NSaffect experiments which explore the QCD phase transition?

It certainly would! And more thanthis… we would LEARN a lot!



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NOT HEAVY ENOUGH



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NOT HEAVY ENOUGH

TROUBLEWITH FLOW



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NOT HEAVY ENOUGH

TROUBLEWITH FLOW

Purely nuclear EoS



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One of the big unknowns when describingquark matter in NSs is the nuclear equation of state.Favorable: Nucleons (…, diquarks, mesons) as quark correlations



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HADRONS AS QUARK BOUNDSTATES

Problem is attacked in vacuum Faddeev Equations

Baryons as composites of confined quarks and diquarks q-propagator, d-propagator, Bethe-Salpeter-Ampl., Faddeev Ampl.

Γ Ψ

Cloet et al. (2008)Current quark mass dependence of nucleon magnetic moments and radii

Eichmann et al. (2008)The nucleon as a QCD bound state in a Faddeev approach.

Bethe Salpeter Equations

P. Maris (2002)Effective masses of diquarks.

Bhagwat et al. (2007)Flavour symmetry breaking and meson masses



20.5.2011

HADRONS AS QUARK BOUNDSTATES

Problem is attacked in vacuum Faddeev Equations

Baryons as composites of confined quarks and diquarks q-propagator, d-propagator, Bethe-Salpeter-Ampl., Faddeev Ampl.

Γ Ψ

Cloet et al. (2008)Current quark mass dependence of nucleon magnetic moments and radii

Eichmann et al. (2008)The nucleon as a QCD bound state in a Faddeev approach.

Bethe Salpeter Equations

P. Maris (2002)Effective masses of diquarks.

Bhagwat et al. (2007)Flavour symmetry breaking and meson masses

But barely explored in

medium



20.5.2011

One of the big unknowns when describing quark matter in NSsis the nuclear equation of state.Favorable: Nucleons (… and diquarks … and mesons!!!) as quark correlations

In medium… this is a challenge we have to face now and in the future.

Work around: model nuclear and free quark matter EoS independently construct a phase transition

A phase transition softens the equation of state!


ADJUSTING THE QUARK MATTER EOS

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Work around: model nuclear and quark matter independently construct a phase transition

A phase transition softens the equation of state! VERY GOOD!!! Solves some problems.


20.5.2011




Work around: model nuclear and quark matter independently construct a phase transition

A phase transition softens the equation of state! VERY GOOD!!! Solves some problems.


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Doesn’t look very systematic



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no stable hybridsPT at too large n



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Quark Stars?PT at too small n



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PSR J1614

sunmax M)04.097.1(M



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PSR J1614

sunmax M)04.097.1(M

Mm

ax increases



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PSR J1614

sunmax M)04.097.1(M

Mm

ax increases

Massive

Quark Cores are HERE



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PSR J1614

Comparison with sym. matter:

QM in PSR J1614?Yes -> No -> It is remarkable thatthis critical value israther constant!Still: For this model…

sunmax M)04.097.1(M

Mm

ax increases

symonsetn

satsymonset 4nn

satsymonset 4nn

Massive

Quark Cores are HERE


CONCLUSIONS

20.5.2011

• Compact Stars provide increasingly severe constraints on the cold EoS• In combination with HIC data it might soon be possible to pin the EoS• Attack EoS already now from both sides and point out model inconsistencies Example here: PSR J1614 vs Flow = EoS neither too soft nor too stiff

• Quark matter in compact stars is NOT ruled out by large masses

• Transport properties and all aspects of temporal evolution will be important

• Consistent approaches are required (A.Sedrakian!)

• We expect an increase of NS data by an order of magnitude

Good times ahead!

Thomas Klähn D. Blaschke R. Łastowiecki F. Sandin 20.5.2011Thomas Klähn – Three Days on...

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