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Thomas Klähn – Three Days on Quarkyonic Island
Thomas Klähn
D. Blaschke
R. Łastowiecki
F. Sandin
20.5.2011
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
CONCLUSION
of the “CompStar School and Workshop” (Catania - May 3-12, 2011)
The most exciting news of the last year:
• Mass of Pulsar J1614-2230 : M  (1.97  0.04)Msun Demorest et al., Nature 467, 1081-1083 (2010)
• Rapid cooling of Cas A
Heinke, Ho, Astrophys. J. Lett., 719, L167 (2010)
Page, Prakash, Lattimer, Steiner, Phys.Rev.Lett.106:081101 (2011)
Blaschke, Grigorian, Prog.Part.Nucl.Phys. 59 (2007)
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
CONCLUSION
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 : M  (1.97  0.04)Msun P.Demorest et al., Nature 467, 1081-1083 (2010)
What are the consequences for the existence of quark matter in Compact Stars?
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
PSR J1614-2230
‫ ہ‬Binary system in Scorpius
‫ ہ‬1200 parsecs from Earth
‫ ہ‬Neutron star with white dwarf companion
‫ ہ‬NS - millisecond pulsar (P=3.15 ms)
‫ ہ‬Time signal is getting delayed when passing near massive object.
‫ ہ‬General relativistic effect.
‫ ہ‬Size of the effect depends on the mass and inclination angle.
‫ ہ‬Pulse delay best to measure when pulsar is exactly behind companion
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
PSR J1614-2230
‫ ہ‬Binary system in Scorpius
‫ ہ‬1200 parsecs from Earth
‫ ہ‬Neutron star with white dwarf companion
‫ ہ‬NS - millisecond pulsar (P=3.15 ms)
‫ ہ‬Recycled pulsar – accretion
‫ ہ‬Time signal is getting delayed when passing near massive object.
‫ ہ‬General relativistic effect.
‫ ہ‬Size of the effect depends on mass and inclination angle.
‫ ہ‬Pulse delay best to measure when pulsar is exactly behind companion
Thomas Klähn – Three Days on Quarkyonic
Island
PSR J1614-2230
Observational Results:
‫ ہ‬89.17 inclination angle
‫ ہ‬companion mass of 0.5 solar masses.
‫ ہ‬companion is a helium-carbon-oxygen white dwarf
20.5.2011
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
PSR J1614-2230
Observational Results:
‫ ہ‬89.17 inclination angle
‫ ہ‬companion mass of 0.5 solar masses.
‫ ہ‬companion is a helium-carbon-oxygen white dwarf
‫ ہ‬neutron star mass:
M  (1.97  0.04)Msun
WORLD (universal? intergalactic?) RECORD!
P.Demorest et al., Nature 467, 1081-1083 (2010)
‫ ہ‬Highest well known mass of NS before:
1.66M sun
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Nuclear matter far beyond saturation density is not well understood:
Klähn et al., Phys.Rev. C74 (2006) 035802
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Large neutron star masses (about 2MSun and more) provide a serious constraint.
Klähn et al., Phys.Rev. C74 (2006) 035802
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Klähn et al., Phys.Rev. C74 (2006) 035802
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
INTERESTING!!!
If UB confirmed
unambiguously...
HIC can constrain
maximum NS
mass!
... which we
estimated quite a
time ago:
M max  2.0  2.1Msun
Klähn et al.,
Phys.Rev. C74 (2006) 035802
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
PSR J1614 AND QUARK MATTER
Can QM be present in PSR J1614?
Presently, one cannot know
whether quark matter exists in
PSR J1614.
However, if there is NO
quark matter in this object,
it is in no other NS we know.
Why is this so?
The more massive a NS is
the higher is the central density.
Would clarifying the question of QM in NS
affect experiments which explore the
QCD phase transition?
It certainly would! And more than
this… we would LEARN a lot!
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
NOT HEAVY
ENOUGH
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
TROUBLE
WITH FLOW
NOT HEAVY
ENOUGH
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
TROUBLE
WITH FLOW
NOT HEAVY
ENOUGH
Purely nuclear EoS
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
One of the big unknowns when describing
quark matter in NSs is the nuclear equation of state.
Favorable: Nucleons (…, diquarks, mesons) as quark correlations
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Problem is attacked in vacuum Faddeev Equations
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.
Baryons as composites of confined quarks and diquarks
q-propagator,
d-propagator, Γ Bethe-Salpeter-Ampl., Ψ Faddeev Ampl.
Bethe Salpeter Equations
P. Maris (2002)
Effective masses of diquarks.
Bhagwat et al. (2007)
Flavour symmetry breaking
and meson masses
HADRONS AS QUARK BOUNDSTATES
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
Problem is attacked in vacuum Faddeev Equations
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.
Baryons as composites of confined quarks and diquarks
q-propagator,
d-propagator, Γ Bethe-Salpeter-Ampl., Ψ Faddeev Ampl.
Bethe Salpeter Equations
P. Maris (2002)
Effective masses of diquarks.
Bhagwat et al. (2007)
Flavour symmetry breaking
and meson masses
HADRONS AS QUARK BOUNDSTATES
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
WHY PSR J1614 IS SO EXCITING
One of the big unknowns when describing quark matter in NSs
is 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!
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
One of the big unknowns when describing quark matter in NSs
is 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 quark matter independently
construct a phase transition
A phase transition softens the equation of state! VERY GOOD!!! Solves some problems.
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
One of the big unknowns when describing quark matter in NSs
is 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 quark matter independently
construct a phase transition
Doesn’t look very systematic
A phase transition softens the equation of state! VERY GOOD!!! Solves some problems.
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Quark Stars?
PT at too small n
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Quark Stars?
PT at too small n
PSR J1614
M max  (1.97  0.04)Msun
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Quark Stars?
PT at too small n
PSR J1614
M max  (1.97  0.04)Msun
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Quark Stars?
PT at too small n
PSR J1614
M max  (1.97  0.04)Msun
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Quark Stars?
PT at too small n
PSR J1614
M max  (1.97  0.04)Msun
Massive
Quark Cores are
HERE
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
ADJUSTING THE QUARK MATTER EOS
no stable hybrids
PT at too large n
Quark Stars?
PT at too small n
PSR J1614
M max  (1.97  0.04)Msun
Comparison with
sym. matter: n sym
onset
QM in PSR J1614?
n sym
Yes ->
onset  4n sat
n sym
No ->
onset  4n sat
It is remarkable that
this critical value is
rather constant!
Still: For this model…
Massive
Quark Cores are
HERE
Thomas Klähn – Three Days on Quarkyonic
Island
20.5.2011
CONCLUSIONS
• 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!