New States of Strongly Interacting Astrophysical Matter

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New States of Strongly Interacting Astrophysical
Matter

• PITP Conference 2005

Mannque Rho (Saclay)
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Where does the mass come from?
Molecules, Atoms, Nuclei Masses sum of masses
of constituents tiny binding
energy Constituents protons, neutrons,
electrons
Nuclear BE lt 1
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Mysteries abound in the Standard Model and Beyond

• Where do the quark, lepton etc. masses come from?
• .. Etc
• Where do the dark stuff in the Universe come
  from?
• .. Etc

For someone else!
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Mass right around us

• Proton/Neutron Mass938/940 MeV

Constituents Quarks and gluons

• Proton uud Neutron udd

Sum of current-quark masses 10 MeV
Where do 99 of the mass come from?
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QCD Answer

• QCD on lattice explains the proton mass
• within 10 .

Energy stored in the motion of the
(nearly) massless quarks and energy in
massless gluons that connect them
Proton mass 1 GeV
Mass without mass

• Technically, chiral symmetry
• spontaneously broken (cSB)

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Order Parameter
_
Quark condensate ltqqgt
? 0 cS broken 0 cS restored
_

• ltqqgt - (0.230.03 GeV)3? Proton
• mass 1 GeV
• What happens when ltqqgt? 0 ?

_
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The Question
If the mass is generated by dynamical dressing,
can it be made to disappear by undressing in
the laboratories ?
Or can one dial the mass to zero?
Yes! through dialing the condensate to zero
Lattice QCD
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(Two) Surprises
New unexpected states are found

• At High Density (Gravity)
• Kaon condensation
• At High Temperature (Heavy-Ion Collisions)
• Nearly perfect liquid

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Effective Field Theories
QCD cannot address directly the problem of going
toward the critical point Tc/nc, so we need to
resort to effective field theories

• Tools at our disposal
• NLs Nonlinear sigma model with pseudo-
• Goldstone bosons (p, K, )
• HLS Hidden local symmetry model
• with p, K, light vectors (r,w,K, )
• etc

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In Favor of HLS

• AdS/QCD indicates a 5-D pure gauge theory
• giving in 4-D a tower of vector mesons and
• a multiplet of Goldstone bosons describing
• QCD in nonperturbative regime
• Baryons emerge as skyrmions to complete
• the degrees of freedom required
• With a suitable truncation and in the chiral
• limit (quark masses0), the theory can arrive
• at the critical point as a fixed point known
• as Vector Manifestation (VM)

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Predictions with HLS
As ltqqgt? 0, i.e., n (or T)? nc (or Tc)

• Theory well defined at this limit!
• Hidden gauge coupling g ? ltqqgt ? 0
• Pion decay constant fp F(ltqqgt) ? 0
• Even away from the limit, hadron mass
• (except for ps) satisfies BR scaling
• e.g., in density
• m(n)/m(0) fp (n)/fp (0) for n n0
• 
  g(n)/g(0) for n gt n0
• where n0 0.16 fm-3 nuclear
  matter

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Nature
There are indications that the scaling is
operative up to n0
mw (n0)/mw fp(n0)/fp 0.8
Bonn CBELSA/TAPS Collaboration gA?wX?p0gX
KEK Deeply bound pionic nuclei
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High precision measurements at GSI from 2007
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A dense new state above n0
It is certain that the interior of neutron
stars is much denser than nuclear matter Can one
create such a dense system in the laboratories?
Answer (T. Yamazaki et al, KEK) Capture
anti-strangeness (e.g. K- ) inside nuclei
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Mechanism
Turns out to be surprisingly simple
Huge attraction from two main sources

• Attractive K- - nuclear interaction

K
? - (1/fp)2 ? density - A
w
A

• Density counters EcSB, tending to restore cS

? - c SKN ? density - B
AB 200 MeV at n ? n0 0.16 fm-3
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Kaon Potential
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Discovery of strangeness nugget
KEK 2004
A bound pnnK S0 (3115)
BEmp 2mn mK mS 194 5 MeV
Average density 3 n0
Strong binding overcomes compression energy!
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Embed K-
Schematic calculation
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Producing Dense Strange Matter
Capture K-s
Yamazaki et al. (future)
ppn
ppnK
ppnKK
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Kaon condensation in neutron stars
How the nugget is stabilized is not yet
understood. However if the same mechanism is
applied to (infinite) neutron star matter,
kaons will condense
mK
me
e- ? K- n
nC nNugget
n
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Observation
For a suitable set of parameters, kaon
condensation occurs at a density slightly above
that of the nugget S0 (3115) . It has one proton
and two neutrons per each condensed kaon just
like the S0 (pnnK-) .
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Consequences

• Kaons condense before chiral symmetry is restored
  and before color superconductivity can set in.
• Condensed kaons soften EOS. An intriguing
  possibility a la Bethe and Brown Compact stars
  with mass greater than 1.5 times the solar mass
  undergo gravitational collapse ? maximum stable
  neutron star mass 1.5 ? solar mass.
• So far no strong cases against the BB scenario
  exists.

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Probing the Early Universe By Heavy
Ions
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Ideal liquid above Tc (?)

State of matter 10-6 s after the Big
Bang
Heavy Ion
Standard lore based on asymptotic
freedom Weakly-coupled quark-gluon
plasma above Tc
(CERN announcement)
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Lattice calculation RHIC experiments indicate
Not a gas of quarks and gluons but

• A strongly coupled system
• much like black hole horizons

• Possibly an ideal liquid
• with viscosity/entropy
• ?h/s 1/4p, 400 times
• smaller than (h/s)water.

• Just above TC , strongly bound
• states of light p, s, r, a1
• saturate the entropy.

Conjectured bound (a la Kovtun, Son and
Starinets) based on holgraphic duality
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Discoveries

• Perfect liquid at Tc e,
• resembling strong
• coupling condensed matter
• systems as well as black hole
• horizons.

• Dense strange nugget at gt 3 n0
• resembling a cluster in kaon
• condensed neutron stars.

Future