New States of New States of Strongly Strongly

Interacting Interacting Astrophysical Astrophysical

MatterMatterPITP Conference 2005PITP Conference 2005

Mannque Rho (Saclay)

Where does the mass Where does the mass come from?come from?

Molecules, Atoms, Nuclei: Masses =sum of masses of constituents + tiny binding energy Constituents: protons, neutrons, electrons

Nuclear BE < 1%

Mysteries abound in the Mysteries abound in the Standard Model and Standard Model and

Beyond…Beyond…

Where do the quark, lepton etc.Where do the quark, lepton etc. masses come from?masses come from?

.. Etc….. Etc… Where do the “dark stuff” in the Where do the “dark stuff” in the

Universe come from?Universe come from? .. Etc….. Etc…

For someone else!

Mass right around usMass right around us

•Proton/Neutron Mass=938/940 MeV

Constituents: Quarks and gluons

• Proton= uud ; Neutron= udd

Sum of “current-quark” masses ≈ 10 MeV

Where do ~ 99% of the mass come from?

QCD Answer QCD Answer

“ 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 SB)”

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

Order ParameterOrder Parameter

Quark condensate: <qq>_

• <qq> ≈ - (0.23±0.03 GeV)3→ Proton mass ≈ 1 GeV• What happens when <qq>→ 0 ?

≠ 0 S broken= 0 S restored

_

_

The QuestionThe 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 thecondensate to zero

LatticeQCD

(Two) Surprises(Two) Surprises

• At High Density (Gravity): Kaon condensation

• At High Temperature (Heavy-Ion Collisions): Nearly perfect liquid

New “unexpected” states are found

Effective Field TheoriesEffective Field Theories

QCD cannot address directly the problem ofgoing toward the critical point Tc/nc, so weneed to resort to effective field theories

Tools at our disposal: • NLNonlinear sigma model with pseudo- Goldstone bosons (K, …) • HLS: Hidden local symmetry model with light vectors (K*, …)etc …

In Favor of HLSIn 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 masses=0), the theory can arrive at the critical point as a fixed point known as “Vector Manifestation (VM)”

Predictions with HLSPredictions with HLS

As <qq>→ 0, i.e., n (or T)→ nc (or Tc)

Theory well defined at this limit! Hidden gauge coupling g <qq> → 0 Pion decay constant fF(<qq>) → 0 Even away from the limit, hadron mass (except for ’s) satisfies “BR scaling”; e.g., in density m(n)/m(0) ≈ fn)/ffor n ≤ n0

≈ g(n)/g(0) for n > n0

where n0 = 0.16 fm-3 nuclear matter

¯¯

¯

NatureNature

There are indications thatthe scaling is operative up to n0

mn0)/m≈ fn0)/f≈ 0.8

Bonn: CBELSA/TAPS CollaborationA→X→+X’

KEK:Deeply boundpionic nuclei

High precision measurements at GSI from 2007

A dense new state above A dense new state above nn00

It is certain that the interior of neutron starsis 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

MechanismMechanismTurns out to be surprisingly simple

Huge attraction from two main sources:• Attractive K- - nuclear interaction

K

A

- (1/fdensity ≡ - A

• Density counters ESB, tending to restore S

- c KN density ≡ - B

A+B ~ 200 MeV at n n0 =0.16 fm-3

Kaon Potential

Discovery of strangeness Discovery of strangeness nuggetnugget

A bound pnnK – = “ S0 (3115)” BE=mp + 2mn + mK – mS

=194 ± 5 MeV

Average density ~ 3 n0

KEK 2004

Strong binding overcomescompression energy!

Embed K-

Schematic calculation

Producing Dense Strange Matter Capture K-’s

Yamazaki et al. (future)

ppn

ppnK

ppnKK

Kaon condensation in Kaon condensation in neutron starsneutron 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*

e

e- → K- + nC ≥ nNugget

n

ObservationObservation

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-) .

ConsequencesConsequences

Kaons condense before chiral symmetry is Kaons condense before chiral symmetry is restored and before color superconductivity restored and before color superconductivity can set in.can set in.

Condensed kaons soften EOS. An intriguing Condensed kaons soften EOS. An intriguing possibility a la Bethe and Brown: Compact possibility a la Bethe and Brown: Compact stars with mass greater than ~ 1.5 times the stars with mass greater than ~ 1.5 times the solar mass undergo gravitational collapse solar mass undergo gravitational collapse maximum stable neutron star mass ~ 1.5 maximum stable neutron star mass ~ 1.5 solar mass. solar mass.

So far no strong cases against the BB So far no strong cases against the BB scenario exists.scenario exists.

“Probing” the Early Universe By Heavy Ions

Ideal liquid above Ideal liquid above TTc c (?)(?)

Standard lore based on asymptotic freedom: Weakly-coupled quark-gluon plasma above Tc

(CERN announcement)

State of matter 10-6 s after the “Big Bang”:

Heavy Ion

Lattice calculation & RHIC experiments indicate: Not a gasof quarks and gluons but

• Possibly an “ideal” liquid with viscosity/entropy /s ~ 1/4*, ~ 400 times smaller than (/s)water.

• A strongly coupled system much like black hole horizons

• Just above TC , strongly bound states of light a1

saturate the entropy.

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

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

Discoveries

Dense strange nugget at > 3 n0

resembling a cluster in kaon condensed neutron stars.

Future