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Correlation femtoscopy R. Lednický, JINR Dubna & IP ASCR Prague. History QS correlations & Multiboson effects FSI correlations Correlation asymmetries Spin correlations Summary. Reviews, books. M.I. Podgoretsky, Sov. J. Part. Nucl. 20 (1989) 266; ЭЧАЯ 20 (1989) 628. - PowerPoint PPT Presentation
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4-6.02.2006 R. Lednický dwstp'06 1
Correlation femtoscopy R. Lednický, JINR Dubna & IP ASCR Prague
• History• QS correlations & Multiboson effects• FSI correlations • Correlation asymmetries• Spin correlations• Summary
4-6.02.2006 R. Lednický dwstp'06 2
Reviews, booksM.I. Podgoretsky, Sov. J. Part. Nucl. 20 (1989) 266; ЭЧАЯ 20 (1989) 628
D.H. Boal et al., Rev. Mod. Phys. 62 (1990) 553
U.A. Wiedemann, U. Heinz, Phys. Rep. 319 (1999) 145
T. Csorgo, Heavy Ion Phys. 15 (2002) 1
R. Lednicky, Phys. Atom. Nucl. 67 (2004) 72
M. Lisa et al., Ann. Rev. Nucl. Part. Sci. 55 (2005) 357
R.M. Weiner, B-E correlations and subatomic interference, John Wiley & sons, LTD
3
History
GGLP’60: observed enhanced ++ , vs +
measurement of space-time characteristics R, c ~ fm
KP’71-75: settled basics of correlation femtoscopy
• proposed CF= Ncorr /Nuncorr & mixing techniques to construct Nuncorr
• clarified role of space-time characteristics in various production models• noted an analogy Grishin,KP’71 & differences KP’75 with
HBT effect in Astronomy (see also Shuryak’73, Cocconi’74)
Correlation femtoscopy :
in > 20 papers
at small opening angles – interpreted as BE enhancement
of particle production using particle correlations
4-6.02.2006 R. Lednický dwstp'06 4
QS symmetrization of production amplitude momentum correlations in particle physics
CF=1+(-1)Scos qx
p1
p2
x1
x2
q = p1- p2 , x = x1- x2nnt , t
, nns , s
2
1
0 |q|
1/R0
total pair spin
2R0
KP’75: different from Astronomy where the momentum correlations are absentdue to “infinite” star lifetimes
5
Intensity interferometry of classical electromagnetic fields in Astronomy HBT‘56 product of single-detector currentscf conceptual quanta measurement two-photon counts
p1
p2
x1
x2
x3
x4
stardetectors-antennas tuned to mean frequency
Correlation ~ cos px34
|p|-1
|x34|
Space-time correlation measurement in Astronomy source momentum picture |p|=|| star angular radius ||
orthogonal tomomentum correlation measurement in particle physics source space-time picture |x|
KP’75 no info on star lifetimeSov.Phys. JETP 42 (75) 211 & longitudinal size
no explicit dependenceon star space-time size
4-6.02.2006 R. Lednický dwstp'06 6
momentum correlation (GGLP,KP) measurements are impossiblein Astronomy due to extremely large stellar space-time dimensions
space-time correlation (HBT) measurements can be realized also in Laboratory:
while
Phillips, Kleiman, Davis’67:linewidth measurement from a mercurury discharge lamp
900 MHz
t nsec
Goldberger,Lewis,Watson’63-66Intensity-correlation spectroscopy Measuring phase of x-ray scattering amplitude
& spectral line shape and widthFetter’65
Glauber’65
Michelson cf HBT interferometers
IA ~ | iexp[i(i+kixA)] |2
~ N+ 2 i<j cos[(i- j)+(ki-kj)xA] Product of intensities averaged over ’s:IA IB =IAIB[1+(2/N2)i<jcos(kijxAB)]
=IAIB [1+|(xA-xB)|2]
Actually measured product of electric currents after filters (0<|i-j|<F) integrated in a time T
ST=∫dt JA JB ~ (Ne2/) T |(0,xA-xB)|2
normalized to r.m.s.(ST) ~ Ne (T/F)1/2
Field intensity in antenna A:
A
IA+B ~ |iexp[i(i+kixA)] + jexp[i(j+kjxB)]|2= 2N+ 2Reiexp[ki(xA-xB)]
IA+B = IA+IB[1+Re(xA-xB)] Fourier transform exp[ik(xA-xB)](k)d4k
B
filter
filter
Required ST /r.m.s.(ST) > 1 T > (2 /Ne)2/F
4-6.02.2006 R. Lednický dwstp'06 8
HBT paraboloid mirrors focusing the light from a star on photomultipliers
4-6.02.2006 R. Lednický dwstp'06 9
(1954) A new type of interferometer for use in radio astronomy
L. Mandel and E. Wolf (1995): Optical coherence and quantum optics
J. Perina (1984): Quantum statistics of linear and nonlinear phenomena
(1956) Correlation between photons in two coherent beams of light
(1956) A test of a new type of stellar interferometer on Sirius
(1956) The question of correlations between photons in coherent light rays
+ E.M. Purcell (1956)
R. Hanbury Brown and R.Q. Twiss:
4-6.02.2006 R. Lednický dwstp'06 10
ST / ST2- ST 2 ½
Normalized to 1 at d=0
Ne ~ 108 e/sec, f ~ 1013 Hz, fF ~ 5-45 MHz
Required T ~ (2 /Ne)2/F ~ hours
HBT measurement of the angular size of Sirius
4-6.02.2006 R. Lednický dwstp'06 11
Coincidence measurements
A. Adam, L. Janossy, P. Varga (1955) 1011 yearsE. Brannen, H.I.S. Ferguson (1956) 103 years
HBT (1956) minutes-hours
Required time
compare to HBT technique
E.M. Purcell: Brown and Twiss did not count individual photoelectrons and coincidences, and were able to work with a primary photoelectric current some 104 times greater than that of Brannen and Ferguson. … This onlyadds lustre to the achievement of Brown and Twiss.
F.T. Arechi, E. Gatti, A. Sona (1966) hours B.L. Morgan, L. Mandel (1966) hours
12
Formal analogy of photon correlationsin astronomy and particle physics
Grishin, Kopylov, Podgoretsky’71:for conceptual case of 2 monochromatic sources and 2 detectors
R and d are distance vectors between sources and detectorsprojected in the plane perpendicular to the emission direction
Correlation ~ cos(Rd/L)
“…study of energy correlation allows one to get information about the source lifetime, and study of angular correlations – about its spatial structure. The latter circumstance is used to measure stellar sizes with the help of the Hanbury Brown & Twiss interferometer.”
correlation takes the same form both in astronomy and particle physics:
L >> R, d is distance between the emitters and detectors
13
The analogy triggered misunderstandings: Shuryak’73: “The interest to correlations of identical quanta is due
Cocconi’74: “The method proposed is equivalent to that used …
“For a stationary source
of the measurement of star radii.”
! Correlation(q) = cos(q d)
Grassberger’77 (ISMD):
case the opposite happens”“While .. interference builds up mostly .. near the detectors .. in our
! Same mistake: many others ..
astronomy and is the basis of Hanbury Brown and Twiss methodstructure of the source of quanta. This idea originates from radioto the fact that their magnitude is connected with the space and time
is the standard one |q d| 1”condition for interference(such as a star) the
… by radio astronomers to study angular dimensions of radio sources”
4-6.02.2006 R. Lednický dwstp'06 14
GGLP effect often called HBT, though:
• HBT did not count quanta – they measured the product of currents ( field intensities) from two antennas – intensity interferometry -
useless technique for correlation femtoscopy• Being of classical origin (Superposition Principle), HBT
effect would survive when h 0 and quantum interference vanished
• Even if quanta measurement were done in Astronomy, it would be orthogonal to that of GGLP
4-6.02.2006 R. Lednický dwstp'06 15
GGLP’60 data plotted as CF
GGLP data plotted as KP CF=N(++,--)/N(+-)
0 0.1 0.2Q2= -(p1-p2)
2 (GeV/c)2
0
1
3
2
Lorstad JMPA 4 (89) 286
R0~1 fm
p p 2+ 2 - n0
4-6.02.2006 R. Lednický dwstp'06 16
Examples of present data: NA49 & STAR
3-dim fit: CF=1+exp(-Rx2qx
2 –Ry2qy
2 -Rz
2qz2
-2Rxz2qx qz)
z x y
Correlation strength or chaoticity
NA49
Interferometry or correlation radii
KK STAR
Coulomb corrected
“General” parameterization at |q| 0
Particles on mass shell & azimuthal symmetry 5 variables:q = {qx , qy , qz} {qout , qside , qlong}, pair velocity v = {vx,0,vz}
Rx2 =½ (x-vxt)2 , Ry
2 =½ (y)2 , Rz2 =½ (z-vzt)2
q0 = qp/p0 qv = qxvx+ qzvz
y side
x out transverse pair velocity vt
z long beam
Podgoretsky’83; often called cartesian or BP’95 parameterization
Interferometry or correlation radii:
cos qx=1-½(qx)2+.. exp(-Rx2qx
2 -Ry2qy
2 -Rz
2qz2 -2Rxz
2qx qz)
Grassberger’77RL’78
Formalism of independent one-particle sourcesx|A = (2)-4 d4 uA() exp[-i (x-xA)]|x = exp(i x)|A = d4x |xx|A = uA() exp(i xA)
Momentum (femtoscopic) correlations:Ampl(p) = p|A = uA(p) exp(i pxA)Ampl(p1,p2) = 2-1/ 2 [uA(p1)uA(p2) exp(i p1xA+i p2xB) + 1 2]Corr(p1,p2) = 2Re{exp(i qx) uA(p1)uB(p2)uA
*(p2)uB*(p1) x
x [|uA(p1)uB(p2)| 2 +|uA(p2)uB(p1)|2]-1 } cos[(p1-p2)(xA-xB)]
Space-time (spectroscopic) correlations:Ampl(x) = x|A ~ exp[i pA(xA-x)] for ~ monochrom. sourceAmpl(x3,x4) ~ exp{i pA(xA-x3)+i pB (xB-x4)] + 3 4}
Corr(x3,x4) ~ cos[(pA-pB )(x3-x4)] ! No explicit dependence on xA, xB
4-6.02.2006 R. Lednický dwstp'06 19
Femtoscopy through Emission function G(p,x)
E d3N/d3p = |T(p)|2 = d4x d4x’ exp[-i p(x-x’)] (x)*(x’)One particle:
= d4x G(p,x) x,x’ x=½(x+x’), =x-x’ G(p,x) = partial Fourier transform of space-time
density matrix (x)*(x’)Two id. pions:
E1E2d6N/d3p1d3p2 = d4x1d4x2 [G(p1,x1;p2,x2)+ G(p,x1;p,x2)cos(qx)]p = ½(p1+p2) q = p1-p2 x = x1-x2
Corr(p1,p2) = d4x1d4x2G(p,x1;p,x2) cos(qx) / d4x1d4x2G(p1,x1;p2,x2) cos(qx) exp(- i Ri
2qi2 - 2q0
2) if G(p1,x1;p2,x2)= G(p1,x1)G(p2,x2) G(p,x) ~ exp(- i xi
2/2Ri2- x0
2/22)
20
Assumptions to derive KP formula
CF - 1 = cos qx
- two-particle approximation (small freeze-out PS density f)
- smoothness approximation: Remitter Rsource |p| |q|peak
- incoherent or independent emission
~ OK, <f> 1 ? low pt fig.
~ OK in HIC, Rsource2 0.1 fm2 pt
2-slope of direct particles
2 and 3 CF data consistent with KP formulae:CF3(123) = 1+|F(12)|2+|F(23)|2+|F(31)|2+2Re[F(12)F(23)F(31)]CF2(12) = 1+|F(12)|2 , F(q)| = eiqx
- neglect of FSIOK for photons, ~ OK for pions up to Coulomb repulsion
21
Phase space density from CFs and spectra
Bertsch’94
May be high phase space density at low pt ?
? Pion condensate or laser
? Multiboson effects on CFsspectra & multiplicities
<f> rises up to SPSLisa ..’05
Multiboson effects Coherent emission: pion laser, DCC … Correlation strength < 1 due to coherence Fowler-Weiner’77
But: impurity, Long-Lived Sources (LLS), .. Deutschman’78
3 CF normalized to 2 CFs: get rid of LLS effect Heinz-Zhang’97 But: problem with 3 Coulomb & extrapolation to Q3=0
Coherence modification of FSI effect on 2 CFs Akkelin ..’00 But: requires precise measurement at low Q
Chaotic emission: Podgoretsky’85, Zajc’87, Pratt’93 .. See RL et al. PRC 61 (00) 034901 & refs therein & Heinz .. AP 288 (01) 325
Widening of n distribution:
Increasing PSD:Poisson BE
Narrowing of spectrum:
/(2r0) < Widening of CFs:
width = 1/r0
= 1width
0 at fixed n
rare gas BE condensate
RL-Podgoretsky’79
4-6.02.2006 R. Lednický dwstp'06 23
3 data on chaotic fraction
Periph Mid-centr Centr
Within large (systematic) errors STAR data is consistent with full chaoticity
r3 =[C3(123) – C2(12) – C2(23) – C2(31) ]/[C2(12) C2(23) C2(31) ]½
C2 = CF2-1 cancel out Heinz-Zhang’97
Interpolate to r3(Q3=0), Q3 = (Q122+ Q23
2+ Q312)½
Construct ratio r3 in which LLS contributions to C3 = CF3-1 and
½r3(0) =½(3-2)/(2-)¾
½r3 STAR’03
2
Full chaoticity
Multiboson effects on n & spectra
Poisson ~ n/n!
BE ~ n
Rare gasWidth=Condensate
Measure of PSD: =/(r0+½)3 1
Width=/(2r0)½
4-6.02.2006 R. Lednický dwstp'06 25
Multiboson effects on CFsCFn(0) fixed n
n
CF(q) inclusive CF(q) semi-inclusive nnmax
nmax
2 120
undershoot
Intercept dropswith n faster
for softer pions
Width logarithmicallyincreases with PSD
Intercept stays at 2
60
n =33.5
4-6.02.2006 R. Lednický dwstp'06 26
Probing source shape and emission duration
Static Gaussian model with space and time dispersions
R2, R||2, 2
Rx2 = R2 +v22
Ry2 = R2
Rz2 = R||
2 +v||22
Emission duration2 = (Rx
2- Ry2)/v2
(degree)
Rsi
de2
fm2
If elliptic shape also in transverse plane RyRside oscillates with pair azimuth
Rside (=90°) small
Rside =0°) large
z
A
B
Out-of reaction plane
In reaction plane
In-planeCircular
Out
-of
plan
e
KP (71-75) …
4-6.02.2006 R. Lednický dwstp'06 27
Probing source dynamics - expansionDispersion of emitter velocities & limited emission momenta (T)
x-p correlation: interference dominated by pions from nearby emitters
Interferometry radii decrease with pair velocity
Interference probes only a part of the sourceResonances GKP’71 ..Strings Bowler’85 ..Hydro
Pt=160 MeV/c Pt=380 MeV/c
Rout RsideRout Rside
Collective transverse flow F RsideR/(1+mt F2/T)½
Longitudinal boost invariant expansionduring proper freeze-out (evolution) time
Rlong (T/mt)½/coshy
Pratt, Csörgö, Zimanyi’90
Makhlin-Sinyukov’87
}1 in LCMS
…..
Bertch, Gong, Tohyama’88Hama, Padula’88
Mayer, Schnedermann, Heinz’92
Pratt’84,86Kolehmainen, Gyulassy’86
Longitudinal boost-invariant expansionel. sources of lifetime produced at t=z=0 uniformly distr. in
t= cosh() z= sinh()E= mt cosh(y) pz= mt sinh(y) E*= mt cosh(y- )
rapidity and decaying according to thermal law exp(-E*/T)
In LCMS: pair rapidity y=0 soG ~ exp(-E*/T)= exp(-mt cosh /T) exp(-mt/T) exp[-2 / 2(T/mt)]
2 (T/mt)
Rz2= (z-z)2 z’2 Ry
2= y’2 Rx2= (x’-vxt’)2
Rz2= ( sinh())2 = 2 (sinh())2 2 (T/mt)
Rx2= x’2-2vxx’t’+vx
2t’2 t’2 (-)2 ()2
Rz = evolution time Rx = emission durationif x’t’=0 & x’2= y’2
4-6.02.2006 R. Lednický dwstp'06 29
Transverse expansion
= exp[ - (0F2 r2/r0
2 + t2 - 2 0
Ft )x/r0) mt / 2T - r2/ 2r02]
Thermal law & gaussian tr. density profile exp(-r2/ 2r02)
& linear tr. flow velocity profile F(r) = 0Fr / r0
Nonrelativistic case: tT2 = F2 + t
2 - 2 Ft cos x = r cos (out) y = r sin (side) t
= tr. velocity tT = tr. thermal velocity
Note: for a box-like profile (r < R) x’2 < y’2
G ~ exp(-tT2 mt / 2T) exp(-r2/ 2r0
2)
y = 0 x = r0 t 0F / [0
F2+T/mt]
Ry2 = y’2 = x’2 = r0
2 / [1+ 0F2 mt /T]
30
AGSSPSRHIC: radii
STAR Au+Au at 200 AGeV 0-5% central Pb+Pb or Au+Au
Clear centrality dependence
Weak energy dependence
31
AGSSPSRHIC: radii vs pt
Rlong:increases smoothly & points to short evolution time ~ 8-10 fm/c
Rside , Rout :change little & point to strong transverse flow 0
F ~ 0.4-0.6 &short emission duration ~ 2 fm/c
Central Au+Au or Pb+Pb
32
Interferometry wrt reaction plane
STAR data: oscillations like for a
static out-of-plane sourcestronger then Hydro & RQMD
Short evolution time
Out-of-plane Circular In-planeTime
Typical hydro evolution STAR’04 Au+Au 200 GeV 20-30% &
4-6.02.2006 R. Lednický dwstp'06 33
hadronizationinitial state
pre-equilibrium
QGP andhydrodynamic expansion
hadronic phaseand freeze-out
PCM & clust. hadronization
NFD
NFD & hadronic TM
PCM & hadronic TM
CYM & LGT
string & hadronic TM
Expected evolution of HI collision vs RHIC data
dN/dt
1 fm/c 5 fm/c 10 fm/c 50 fm/c time
Kinetic freeze outChemical freeze out
RHIC side & out radii: 2 fm/c
Rlong & radii vs reaction plane: 10 fm/c
Bass’02
34
Puzzle ?
3D Hydro
2+1D Hydro
1+1D Hydro+UrQMD
(resonances ?)
But comparing1+1D H+UrQMDwith 2+1D Hydro
kinetic evolution
at small pt
& increases Rside
~ conserves Rout,Rlong
Good prospect for 3D Hydro
Hydro assuming ideal fluid explains strong collective () flows at RHIC but not the interferometry results
+ hadron transport
Bass, Dumitru, ..
Huovinen, Kolb, ..
Hirano, Nara, ..
? not enough F
+ ? initial F
Why ~ conservation of spectra & radii?
qxi’ qxi +q(p1+p2)T/(E1+E2) = qxi
Sinyukov, Akkelin, Hama’02:
free streaming also in real conditions and thus
initial interferometry radii
ti’= ti +T, xi’ = xi + vi T , vi v =(p1+p2)/(E1+E2)
Based on the fact that the known analytical solutionof nonrelativistic BE with spherically symmetricinitial conditions coincides with free streaming
one may assume the kinetic evolution close to
~ conserving initial spectra and
~ justify hydro motivated freezeout parametrizations
Csizmadia, Csörgö, Lukács’98
36
Checks with kinetic modelAmelin, RL, Malinina, Pocheptsov, Sinyukov’05:
System cools
& expands
but initial
Boltzmann
momentum
distribution &
interferomety
radii are
conserved due
to developed
collective flow
~ ~ tens fm = = 0in static model
37
Hydro motivated parametrizations
Kniege’05
BlastWave: Schnedermann, Sollfrank, Heinz’93Retiere, Lisa’04
38
BW fit ofAu-Au 200 GeV
T=106 ± 1 MeV<InPlane> = 0.571 ± 0.004 c<OutOfPlane> = 0.540 ± 0.004 cRInPlane = 11.1 ± 0.2 fmROutOfPlane = 12.1 ± 0.2 fmLife time () = 8.4 ± 0.2 fm/cEmission duration = 1.9 ± 0.2 fm/c2/dof = 120 / 86
Retiere@LBL’05
39
Other parametrizationsBuda-Lund: Csanad, Csörgö, Lörstad’04 Similar to BW but T(x) & (x)hot core ~200 MeV surrounded by cool ~100 MeV shellDescribes all data: spectra, radii, v2()
Krakow: Broniowski, Florkowski’01
Describes spectra, radii but Rlong
Single freezeout model + Hubble-like flow + resonances
Kiev-Nantes: Borysova, Sinyukov, Erazmus, Karpenko’05
closed freezeout hypersurfaceGeneralizes BW using hydro motivated
Additional surface emission introducesx-t correlation helps to desribe Rout
at smaller flow velocity
volume emission
surface emission
? may account for initial F
Fit points to initial 0F of ~ 0.3
4-6.02.2006 R. Lednický dwstp'06 40
Final State InteractionSimilar to Coulomb distortion of -decay Fermi’34:
e-ikr -k(r) [ e-ikr +f(k)eikr/r ]
eicAcF=1+ _______ + …kr+kr
ka
Coulomb
s-wavestrong FSIFSI
fcAc(G0+iF0)}
}
Bohr radius}
Point-likeCoulomb factor k=|q|/2
CF nnpp
Coulomb only
|1+f/r|2
FSI is sensitive to source size r and scattering amplitude fIt complicates CF analysis but makes possible
Femtoscopy with nonidentical particles K, p, .. &
Study relative space-time asymmetries delays, flow Study “exotic” scattering , K, KK, , p, , ..
Coalescence deuterons, ..
|-k(r)|2Migdal, Watson, Sakharov, … Koonin, GKW, ...
Assumptions to derive “Fermi” formula
CF = |-k(r)|2
- tFSI tprod |k*| = ½|q*| hundreds MeV/c
- same as for KP formula in case of pure QS &
- equal time approximation in PRF
typical momentum transfer in production
RL, Lyuboshitz’82 eq. time condition |t*| r*2
OK fig.
RL, Lyuboshitz ..’98
same isomultiplet only: + 00, -p 0n, K+K K0K0, ...
& account for coupledchannels within the
4-6.02.2006 R. Lednický dwstp'06 42
Effect of nonequal times in pair cmsRL, Lyuboshitz SJNP 35 (82) 770; RL nucl-th/0501065
Applicability condition of equal-time approximation: |t*| r*2 r0=2 fm 0=2 fm/c r0=2 fm v=0.1
OK for heavy
particles
OK within 5%even for pions if0 ~r0 or lower
Note: v ~ 0.8
CFFSI(00)
4-6.02.2006 R. Lednický dwstp'06 43
FSI effect on CF of neutral kaons
STAR data on CF(KsKs)
Goal: no Coulomb. But R may go up by ~1 fm if neglected FSI in
= 1.09 0.22R = 4.66 0.46 fm 5.86 0.67 fm
KK (~50% KsKs) f0(980) & a0(980)RL-Lyuboshitz’82 couplings from
t
Achasov’01,03 Martin’77
no FSI
Lyuboshitz-Podgoretsky’79: KsKs from KK also showBE enhancement
4-6.02.2006 R. Lednický dwstp'06 44
NA49 central Pb+Pb 158 AGeV vs RQMDLong tails in RQMD: r* = 21 fm for r* < 50 fm
29 fm for r* < 500 fm
Fit CF=Norm [Purity RQMD(r* Scaler*)+1-Purity]
Scale=0.76 Scale=0.92 Scale=0.83
RQMD overestimates r* by 10-20% at SPS cf ~ OK at AGS worse at RHIC
p
4-6.02.2006 R. Lednický dwstp'06 45
p CFs at AGS & SPS & STAR
Fit using RL-Lyuboshitz’82 with consistent with estimated impurityR~ 3-4 fm consistent with the radius from pp CF
Goal: No Coulomb suppression as in pp CF &Wang-Pratt’99 Stronger sensitivity to R
=0.50.2R=4.50.7 fm
Scattering lengths, fm: 2.31 1.78Effective radii, fm: 3.04 3.22
singlet triplet
AGS SPS STAR
R=3.10.30.2 fm
4-6.02.2006 R. Lednický dwstp'06 46
Correlation study of particle interaction
-
+& & p scattering lengths f0 from NA49 and STAR
NA49 CF(+) vs RQMD with SI scale: f0 sisca f0 (=0.232fm)
sisca = 0.60.1 compare ~0.8 fromSPT & BNL data E765 K e
Fits using RL-Lyuboshitz’82
NA49 CF() data prefer |f0()| f0(NN) ~ 20 fm
STAR CF(p) data point to Ref0(p) < Ref0(pp) 0
Imf0(p) ~ Imf0(pp) ~ 1 fm
pp
47
Correlation study of particle interaction
-
+ scattering length f0 from NA49 CF
Fit CF(+) by RQMD with SI scale: f0 sisca f0
input f0
input = 0.232 fm
sisca = 0.60.1 Compare with
~0.8 from SPT & BNL E765
K e
+
CF=Norm [Purity RQMD(r* Scaler*)+1-Purity]
4-6.02.2006 R. Lednický dwstp'06 48
interaction potential from LEP CF = Norm (1 e-R2Q2)
=0.620.09R=0.110.02 fm
=0.540.10R=0.110.03 fm
=0.600.07R=0.100.02 fm
Pure QS: = ½(1+P2) < 0.3Feed-down & PID: ~ 0.5
Polarization < 0.3 }String picture: lstring~ 2mt/~2 fm ~1 fmRz (T/mt)½ ~ 0.3 fm R > Rz /3 ~ 0.17 fm
QS fit yields too low R & too big
FSI potential core RL (02)
=0.6 fixedR=0.290.03 fm
NSC97eneglected
Spin-orbit &Tensor parts
R OK but potential
tuningrequired
PLB 475 (00) 395
CF at LEP dominated by ! Direct core signal
4-6.02.2006 R. Lednický dwstp'06 49
Correlation asymmetries
CF of identical particles sensitive to terms even in k*r* (e.g. through cos 2k*r*) measures only
dispersion of the components of relative separation r* = r1
*- r2* in pair cms
CF of nonidentical particles sensitive also to terms odd in k*r* measures also relative space-time asymmetries - shifts r*
RL, Lyuboshitz, Erazmus, Nouais PLB 373 (1996) 30 Construct CF+x and CF-x with positive and negative k*-projection
k*x on a given direction x and study CF-ratio CF+x/CFx
4-6.02.2006 R. Lednický dwstp'06 50
Simplified idea of CF asymmetry(valid for Coulomb FSI)
x
x
v
v
v1
v2
v1
v2
k*/= v1-v2
p
p
k*x > 0v > vp
k*x < 0v < vp
Assume emitted later than p or closer to the center
p
p
Longer tint
Stronger CF
Shorter tint Weaker CF
CF
CF
4-6.02.2006 R. Lednický dwstp'06 51
CF-asymmetry for charged particlesAsymmetry arises mainly from Coulomb FSI
CF Ac() |F(-i,1,i)|2 =(k*a)-1, =k*r*+k*r*
F 1+ = 1+r*/a+k*r*/(k*a)r*|a|
k*1/r* Bohr radius
}
±226 fm for ±p±388 fm for +±
CF+x/CFx 1+2 x* /ak* 0
x* = x1*-x2* rx* Projection of the relative separation r* in pair cms on the direction x
In LCMS (vz=0) or x || v: x* = t(x - vtt)
CF asymmetry is determined by space and time asymmetries
4-6.02.2006 R. Lednický dwstp'06 52
Large lifetimes evaporation or phase transitionx || v |x| |t| CF-asymmetry yields time delay
Ghisalberti (95) GANILPb+Nb p+d+X
CF+(pd)
CF(pd)
CF+/CF< 1
Deuterons earlier than protonsin agreement with coalescence
e-tp/ e-tn/ e-td/(/2) since tp tn td
Two-phase thermodynamic
model
CF+/CF< 11 2 3
1
2
3
Strangeness distillation: K earlier than K in baryon rich QGP
Ardouin et al. (99)
4-6.02.2006 R. Lednický dwstp'06 53
ad hoc time shift t = –10 fm/c
CF+/CF
Sensitivity test for ALICEa, fm
84
226
249CF+/CF 1+2 x* /a
k* 0
Here x*= - vt
CF-asymmetry scales as - t/a
Erazmus et al. (95)
Delays of several fm/ccan be easily detected
4-6.02.2006 R. Lednický dwstp'06 54
Usually: x and t comparable RQMD Pb+Pb p +X central 158 AGeV : x = -5.2 fm
t = 2.9 fm/cx* = -8.5 fm+p-asymmetry effect 2x*/a -8%
Shift x in out direction is due to collective transverse flow
RL’99-01 xp > xK > x > 0& higher thermal velocity of lighter particles
rt
y
x
F
tT
t
F= flow velocity tT = transverse thermal velocity
t = F + tT = observed transverse velocity
x rx = rt cos = rt (t2+F2- t
T2)/(2tF) y ry = rt sin = 0 mass dependence
z rz sinh = 0 in LCMS & Bjorken long. exp.
out
side
measures edge effect at yCMS 0
pion
Kaon
Proton
BW Retiere@LBL’05
Distribution of emissionpoints at a given equal velocity: - Left, x = 0.73c, y = 0 - Right, x = 0.91c, y = 0
Dash lines: average emission Rx
Rx() < Rx(K) < Rx(p)
px = 0.15 GeV/c px = 0.3 GeV/c
px = 0.53 GeV/c px = 1.07 GeV/c
px = 1.01 GeV/c px = 2.02 GeV/c
For a Gaussian density profile with a radius RG and flow velocity profile F (r) = 0 r/ RG
RL’04, Akkelin-Sinyukov’96 :
x = RG x 0 /[02+T/mt]
NA49 & STAR out-asymmetriesPb+Pb central 158 AGeV not corrected for ~ 25% impurityr* RQMD scaled by 0.8
Au+Au central sNN=130 GeV corrected for impurity
Mirror symmetry (~ same mechanism for and mesons) RQMD, BW ~ OK points to strong transverse flow
pp K
(t yields ~ ¼ of CF asymmetry)
4-6.02.2006 R. Lednický dwstp'06 57
Spin correlations , tt, ..
p
p
n2
n1
Joint angular distribution of decay analyzers n1 and n2 is determined by:
16²W(n1,n2) = 1+ 1P1n1+ 2P2n2+ 12ikTik n1in2k
Decay asymmetry parameters:1 = 2 = (p) = 0.642
polarization vectors Pi= icorrelation tensor Tik = 1k2k
W(x) = ½[1+ ½ 12SpT x]
Distribution of correlation x = n1n2 = cos12 is determined by SpT = sSpTsinglet + tSpTtriplet = -3 s+ t
= 4 t-3
s and t are singlet and triplet fractions, s+ t
= 1:3Alexander-Lipkin (95), RL (99)
58
spin correlations at LEP ALEPH distributions of
correlation x=n1n2= cos12
of directions of decay protonsSlopes ~ SpT = 4 t-3
New femtoscopy tool: t =t/0 triplet state forbidden at Q=0
Noninteracting unpolarized s Check two-particle QM coherence:
violation of Bell-type inequalityRL-Lyuboshitz (01) SpT 1 t½
t = t/
Q 0
t=¾(1e-r02Q2)
s=¼(1e-r02Q2)
=st
r0=0.140.09 fm
Bell-type inequalityx = cos12
Summary• Assumptions behind femtoscopy theory in HIC seem OK• Wealth of data on correlations of various particle species
(,K0,p,,) is available & gives unique space-time info on production characteristics including collective flows
• Rather direct evidence for strong transverse flow in HIC at SPS & RHIC comes from nonidentical particle correlations
• Weak energy dependence of correlation radii contradicts to 2+1D hydro & transport calculations which strongly overestimate out&long radii at RHIC. However, a good perspective seems to be for 3D hydro ?+ F
initial & transport • A number of succesful hydro motivated parametrizations
give useful hints for microscopic models (but fit true )• Info on two-particle strong interaction: & & p
scattering lengths from HIC at SPS and RHIC. Good perspective at RHIC and LHC
• Promising results from Spin correlations
4-6.02.2006 R. Lednický dwstp'06 60
Apologize for skipping
• Coalescence (new d, d data from NA49)• Beyond Gaussian form RL, Podgoretsky, ..Csörgö .. Chung ..
• Imaging technique Brown, Danielewicz, ..
• Multiple FSI effects Wong, Zhang, ..; Kapusta, Li; Cramer, ..
• Spin correlations Alexander, Lipkin; RL, Lyuboshitz
• ……
Kniege’05
4-6.02.2006 R. Lednický dwstp'06 62
Hydro wrt reaction planeHeinz, Kolb, hep-ph/0111075 Though Hydro
transforms out-of planesource into in-plane one,the expansion dynamics
leads to qualitativelysimilar dependence as
for the static out-of planesource
Quantitative differences:• Rs too small, Ro,l too big• oscill. amplit. too small
63
Finite-size effectsr* ~ 10 fm but ~30-40 fm and ’ ~900 fm
UrQMD: pNi 2 at 24 GeV ~1% ’, ~19%
ML
’
ML ~ r*2/[1+(r*/r0)2a]2b
short-distance parametrization
’ and
contributionswell fitted basedon exponential
decay law
64
DIRAC CF: CF=N{ |-k*(r*)|2SLS +(1- )}[1+s Q]
SLS determined by:
ML(r0,a,b), fML=1-f-f’
’, f’
, f
Nr0 fmabff’s
f = 17 6% ML
G2fm
G3fm
’
4-6.02.2006 R. Lednický dwstp'06 65
=0.89
r*=16 fm
=0.93
r*=24 fm
=0.81
r*=18.4 fm
=0.76
r*=18.1 fm
=0.94
r*=24.4 fm
=0.91
r*=22.9 fm
Tails in RQMD: r* = 21 fm for r* < 50 fm
29 fm for r* < 500 fm
Strong FSI on
>
++
+-
Strong FSI important for +-
1-G fit: (++) 0.8, r* 25% 2-G fit: ++ +-
r*QS < r*Coul
1-G fit
2-G fit
4-6.02.2006 R. Lednický dwstp'06 66
Femtoscopy with nonidentical particles
CF = |-k* (r*)|2Be careful when comparing
QS (++ ..) and FSI correlations (+..) different sensitivity to r*-distribution tails
QS & strong FSI: non-Gaussian r*-tail influences only first few bins in Q=2k* and its effect is mainly
absorbed in suppression parameter Coulomb FSI: sensitive to r*-tail up to r* ~ Bohr radius
|a|=|z1z2e2|-1
fm K p KK pp388 249 223 110 58
In Gaussian fits one may expect r0(++) < r0(+)
Use realistic models like transport codes
4-6.02.2006 R. Lednický dwstp'06 67
Coalescence: deuterons ..
Edd3N/d3pd = B2 Epd3N/d3pp End3N/d3pn pp pn ½pd
WF in continuous pn spectrum -k*(r*) WF in discrete pn spectrum b(r*)
Coalescence factor: B2 = (2)3(mpmn/md)-1t|b(r*)|2 ~ R-3
Triplet fraction = ¾ unpolarized Ns
Usually: n p
Much stronger energy dependenceof B2 ~ R-3 than expected from
pion and proton interferometry radii
B2
R(pp) ~ 4 fm from AGS to SPS
Lyuboshitz (88) ..
4-6.02.2006 R. Lednický dwstp'06 68
collective flow chaotic source motion
x-p correlation yes no
x2-p correlation yes yesTeff with m yes yesR with mt yes yes
x 0 yes noCF asymmetry yes yes if t 0