High energy factorization in Nucleus-Nucleus collisions

Transcription

1 High energy factorization in Nucleus-Nucleus collisions François Gelis CERN and CEA/Saclay François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 1

2 Outline at LO and NLO Expression as variations of the initial fields Leading log divergences and Leading Log factorization (FG, T. Lappi and R. Venugopalan, in preparation) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 2

3 Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 3

4 Saturation domain Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x log(x -1 ) log(q 2 ) Λ QCD François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 4

5 CGC degrees of freedom Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x The fast partons (large x) are frozen by time dilation described as static color sources on the light-cone : J µ a = δ µ+ δ(x )ρ a ( x ) (x (t z)/ 2) Slow partons (small x) cannot be considered static over the time-scales of the collision process they must be treated as the usual gauge fields Since they are radiated by the fast partons, they must be coupled to the current J µ a by a term : A µ J µ The color sources ρ a are random, and described by a distribution functional W Y [ρ], with Y the rapidity that separates soft and hard François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 5

6 CGC evolution Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x Evolution equation (JIMWLK) : W Y [ρ] = H[ρ] W Y Y [ρ] Z δ H[ρ] = σ( x ) δρ( x ) + 1 Z δ 2 χ( x, y 2 ) δρ( x )δρ( y ) x x, y σ and χ are non-linear functionals of ρ This evolution equation resums the powers of α s ln(1/x) and of Q s /p that arise in loop corrections This equation simplifies into the BFKL equation when the color density ρ is small (one can expand σ and χ in ρ) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 6

7 Nucleus-nucleus collisions Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x t freeze out hadrons in eq. gluons & quarks in eq. ideal hydrodynamics gluons & quarks out of eq. viscous hydrodynamics strong fields z (beam axis) classical EOMs calculate the initial production of semi-hard particles provide initial conditions for hydrodynamics François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 7

8 CGC and Nucleus-Nucleus collisions Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x? L = 1 2 trf µνf µν + (J µ 1 + Jµ 2 }{{} )A µ Given the sources ρ 1,2 in each projectile, how do we calculate observables? Is there some kind of perturbative expansion? Loop corrections and factorization? J µ François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 8

9 Initial particle production Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x Dilute regime : one parton in each projectile interact François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 9

10 Initial particle production Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x Dilute regime : one parton in each projectile interact Dense regime : multiparton processes become crucial (+ pileup of many partonic scatterings in each AA collision) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 9

11 What is factorization? Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x A factorization formula divides an observable into a perturbatively calculable part (involving quarks and gluons) and a non-perturbative part describing the partonic content of hadrons or nuclei : O = F O partonic has no predictive power unless the distributions F are intrinsic properties of the incoming projectiles : F cannot depend on the observable F of one projectile cannot depend on the second projectile can accommodate certain resummations : Loop corrections in QCD generate corrections of the form [α s log( )] n, that are large in some parts of the phase-space When these corrections do not depend on the observable and projectiles, they can be absorbed in the definition of F via an universal evolution equation François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 10

12 in the linear regime Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x in the linear small-x regime is known as k T -factorization It was introduced in the discussion of heavy quark production near threshold, when s 4m 2 q, to resum large logs of 1/x 1,2 Collins, Ellis (1991), Catani, Ciafaloni, Hautmann (1991) Levin, Ryskin, Shabelski, Shuvaev (1991) In this framework, cross-sections read : dσ dy d 2 P Z k1, k 2 δ( k 1 + k 2 P ) ϕ 1 (x 1, k 1 ) ϕ 2 (x 2, k 2 ) M 2 k 2 1 k2 2 x 1,2 = M s e ±Y The small-x leading logs are resummed into the non-integrated gluon distributions ϕ 1,2 by letting them evolve according to the BFKL equation François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 11

13 in the nonlinear regime Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x In the nonlinear regime, observables are sensitive to parton correlations beyond 2-point correlations. The distributions ϕ 1,2 do not provide this information, but it is present in the source distributions W[ρ 1,2 ] of the CGC in the nonlinear regime at small-x has been established for DIS. The leading logs can be absorbed into W[ρ] by letting it evolve according to the JIMWLK equation In the collision of two dense projectiles : The large logs have a coefficient that depends in a complicated way on the sources of both nuclei. One must show that they can still be absorbed in one of the two W[ρ] s The dependence of the observable on the sources ρ 1,2 is not known analytically, already at LO Even less is known about loop corrections... François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 12

14 in the nonlinear regime Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x For the single gluon spectrum in AA collisions, one would like to establish a formula such as : fi dn d 3 p fl = LLog with Z ˆDρ1 Dρ 2 WYbeam y [ρ 1] W y+ybeam [ρ 2] Y W Y = H W p dn d 3 p LO Y - Ybeam ρ 2 y ρ 1 + Y beam All the leading logs of 1/x 1,2 should be absorbed in the W s The W s should obey the JIMWLK evolution equation François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 13

15 in four easy steps Parton saturation Color Glass Condensate Nucleus-nucleus collisions at small x I : Express the single gluon spectrum at LO and NLO in terms of classical fields and small field fluctuations. Check that their boundary conditions are retarded II : Write the NLO terms as a perturbation of the initial value of the classical fields on the light-cone : dn d 3 p NLO = h 1 2 Z u, v LC Σ( u, v)ì u Ì v + Z u LC β( u)ì u i dn d 3 p LO III : For u, v on the same branch of the light-cone, one has : 1 2 Z u, v LC Σ( u, v)ì u Ì v + Z u LC β( u)ì u = log Λ + p + H + finite terms IV : These are the only logs. follows trivially François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 14

16 Leading Order Next to Leading Order - I - at LO and NLO François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 15

17 at LO p Leading Order Next to Leading Order Leading Order = tree diagrams only Tag one gluon of momentum p Integrate out the phase-space of all the other gluons dn d 3 p n=0 1 n! [ d 3 p 1 d 3 p n ] p p1 p n 0 2 François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 16

18 at LO Leading Order Next to Leading Order LO results for the single gluon spectrum : Disconnected graphs cancel in the inclusive spectrum At LO, the single gluon spectrum can be expressed in terms of classical solutions of the field equation of motion These classical fields obey retarded boundary conditions dn d 3 p LO = lim t + d 3 xd 3 y e i p ( x y) A µ (t, x) A ν (t, y) [ Dµ, F µν] = J ν lim t Aµ (t, x) = 0 François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 17

19 at LO Retarded classical fields are sums of tree diagrams : Leading Order Next to Leading Order x y François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 18

20 at LO Retarded classical fields are sums of tree diagrams : Leading Order Next to Leading Order x y A Note : the gluon spectrum is a functional of the value of the classical field just above the backward light-cone : dn d 3 p = F[A] François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 18

21 at LO Krasnitz, Nara, Venugopalan ( ), Lappi (2003) Leading Order Next to Leading Order 2 k T )dn/d 2 1/(πR 10-1 KNV I KNV II Lappi k T /Λ s Important softening at small k compared to pqcd (saturation) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 19

22 at NLO p Leading Order Next to Leading Order Next to Leading Order = 1-loop diagrams Connected diagrams only Expressible in terms of classical fields, and small fluctuations about the classical field, both with retarded boundary conditions François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 20

23 at NLO Leading Order Next to Leading Order 1-loop graphs contributing to the gluon spectrum at NLO : x y x y dn d 3 p NLO = lim t + [ d 3 xd 3 y e i p ( x y) G +(x, µν y) ] +β µ (t, x) A ν (t, y) + A µ (t, x) β ν (t, y) G µν + is a 2-point function β µ is a small field fluctuation driven by a 1-loop source François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 21

24 at NLO Leading Order Next to Leading Order The equation of motion for β µ reads ˆDµ, ˆD µ, β ν ˆD µ, ˆD ν, β µ + igˆf µ ν, β µ = = L Y M (A) A ν (x) A ρ (x) A σ (x) {z } G ρσ ++(x, x) 3-gluon vertex in the background A The 2-point functions G µν + and G µν ++ can be written as with G µν +(x, y) = Z G µν ++(x, x) = < : d 3 k η µ (2π) 3 k 2E (x) ην +k(y) k Z d 3 k h i η µ (2π) 3 k 2E (x) ην +k(x) + η µ +k (x) ην k(x) k ˆDµ, ˆD µ, η±k ν ˆDµ, ˆD ν, η µ ±k + ν igˆfµ, η µ ±k = 0 lim t ηµ ±k (t, x) = ǫµ (k) e ±ik x François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 22

25 - II - Expression as a perturbation of the initial classical field François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 23

26 at NLO For a small field fluctuation a µ (not driven by a source) propagating on top of the classical field A µ, one can prove : [ ] a µ Ì (x) = a(u) u A µ (x) u LC LC denotes a surface just above the backward light-cone Ì u is the generator of shifts of the initial value of the fields on this surface : h Z i F[A + a] Ì exp a(u) u F[A] u LC LC Note : this construction is possible only because the objects involved in the problem obey retarded boundary conditions François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 24

27 at NLO 1-loop graphs contributing to the gluon spectrum at NLO : x y x y François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 25

28 at NLO 1-loop graphs contributing to the gluon spectrum at NLO : x y x y u v u v They can be written as a perturbation of the LC initial fields : dn h Z 1 i dn = d 3 Σ( u, v)ì u Ì v p 2 d 3 p NLO Σ( u, v) Z u, v LC d 3 k (2π) 3 2E k η k (u) η +k (v) LO François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 25

29 at NLO 1-loop graphs contributing to the gluon spectrum at NLO : x y x y x y u v u v u The loop correction can also be below the light-cone : dn h Z Z 1 i = d 3 Σ( u, v)ì u Ì v + β( u)ì u p 2 NLO u, v LC u LC dn d 3 p LO the functions Σ( u, v) and β( u) can be evaluated analytically François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 25

30 Divergences Leading Log approximation - III - François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 26

31 Divergences Divergences Leading Log approximation If u, v belong to the same branch of the LC (e.g. u = v = ǫ), the function Σ( u, v) contains Σ( u, v) + 0 dk + k + eik (u + v + ) with k k2 2k + the integral converges at k + = 0 but not when k + + Note : the log is a log(λ + /p + ), where Λ + is the boundary between the hard color sources and the fields, and p + the longitudinal momentum of the produced gluon p Λ + ρ 1 p + Similar considerations apply when u, v both belong to the other branch of the LC, leading to a log(λ /p ) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 27

32 Leading Log approximation Divergences Leading Log approximation In the LC gauge A + = 0, the operator η(u) Ì u is η(u) Ì u ( ηa(u)) i δ δ δ( A i a(u)) +η a (u) δa a (u) +( µη a(u)) µ δ δ( µ A µ a(u)) An explicit calculation of η±k i and η ±k shows that these components have an extra 1/k + when k + + At leading log, it seems sufficient to consider : Ì η(u) u = ( µ η µ δ LLog a(u)) δ( µ A µ a(u)) This is almost correct, but not quite... François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 28

33 Leading Log approximation Divergences Leading Log approximation The space-time above the LC contains a classical background field, A ± = 0, A i = i g Ω i Ω the interaction of the fluctuation with a background field can turn terms that are not divergent on the LC into divergent terms! (factors of k + can arise in the 3-gluon derivative coupling) Because the background is a pure gauge, this problem is circumvented by using Ω ab η b instead of η a as the initial condition : Ì η(u) u ( Ω ab ηb(u)) i δ δ( Ω ab A i b (u)) + Ω abη δ b (u) δω ab A b (u) +( µ Ω ab η µ b (u)) δ δ( µ Ω ab A µ b (u)) at leading log, only the last term matters François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 29

34 Divergences Leading Log approximation The coefficient of the leading log does not depend on u +, v + Derivatives with respect to µ Ω ab A µ b (u) can be mapped to derivatives with respect to the slowest color sources : Z du + δ δ( µ Ω ab A µ b (u)) = with 2 e A + (ǫ, x ) = ρ(ǫ, x ) Z d 2 x u 1 x 2 δ δ e A + a (ǫ, x ) When u, v are on the same branch of the LC, we have 1 2 Z u, v LC «Σ( u, v)ì 1 Λ + Z u Ì v = LLog 2 log η ab( x p +, y ) x, y δ 2 δ e A + a (ǫ, x )δ e A + b (ǫ, y ) with η ab ( x, y ) 1 Z d 2 z ( x z ) ( y z ) π (2π) 2 ( x z) 2 ( y z ) 2 h i 1 + Ω(x)Ω (y) Ω(x)Ω (z) Ω(z)Ω (y) ab François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 30

35 Divergences Leading Log approximation In principle, one could evaluate the term involving β( u) by solving explicitly its EOM Shortcut: by using the Green s formula for this fluctuation, one can show directly that Z u LC β( u)ì 1 Λ + «Z u = LLog 2 log p + x Z y! δη ab ( x, y ) δ e A + b (ǫ, y ) δ δ e A + a (ǫ, x ) Combining the real and virtual terms : h Z Z 1 Σ( u, v)ì u Ì v + 2 β( u)ì u i u, v LC u LC «Λ + Z 1 = log δ LLog p + 2 δa e+ b (ǫ, y ) η δ ab( x, y ) δa e+ a (ǫ, x ) y {z } JIMWLK H François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 31

36 Leading Log divergences - IV - François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 32

37 Leading Log divergences Leading Log divergences The configuration where u, v are on the first branch of the LC can be rewritten as ( ) dn Λ + d 3 = p log dn LLog p + H 1 d 3 p NLO LO with H 1 the for the first nucleus Including also the configuration where both u, v are on the second branch of the LC, we get dn [ ( ) ( ) Λ + Λ ] dn d 3 = log p LLog p + H 1 + log p H 2 d 3 p NLO LO François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 33

38 Leading Log divergences Leading Log divergences The only remaining possibility is to have u and v on different branches of the LC However, there is no log divergence in this case, since the k + integral is of the form : η µ -k(u) η ν +k(v) LC dk + k + eik + (u v ) e ik (u + v + ) no mixing of the divergences of the two nuclei François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 34

39 Leading Log factorization Leading Log divergences All the above discussion is for one given configuration of the sources ρ 1,2 (or of the fields A e± 1,2 ). Averaging over all the configurations of the sources in the two projectiles, and using the hermiticity of the, we get fi fl Z dn = ˆDA e+ d 3 1 DA p e 2 LLog LO+NLO h ««Λ + Λ i 1 + log H 1 + log H 2 p + p W[ A e+ 1 ] W[ A e dn 2 ] d 3 p LO This is a 1-loop result. Using RG arguments, this leads to the following factorized formula for the resummation of the leading log terms to all orders : fi fl Z dn = ˆDA e+ d 3 1 DA p e 2 LLog with WY1 [ e A + 1 ] W Y2 [ e A 2 ] dn d 3 p LO Y W Y = H W, Y 1 = log(p + 1 /p + ), Y 2 = log(p 2 /p ) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 35

40 François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 36

41 Requirements for factorization The fact that the observable is bilinear in the fields is not essential. The formula [ 1 ] Σ( u, v)ì O NLO = u Ì v β( u)ì + u O 2 LO u, v LC u LC can be established for more general observables, provided their expectation value depends on retarded fields only Crucial ingredients for factorization : Only connected diagrams should contribute One should have an initial value problem retarded boundary conditions seem essential The observable should involve only one rapidity scale. Otherwise, there are extra large corrections in α s (y 1 y 2 ) that are not captured in the evolution of the W[ñ ] s François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 37

42 Quantities that do factorize Energy-momentum tensor T µν (τ, η, x ) : T µν (τ, η, x ) = LLog Z ˆD e A + 1 D e A 2 WY1 [ e A + 1 ] W Y2 [ e A 2 ] with Y 1 = Y beam η, Y 2 = Y beam + η CGC initial conditions for hydrodynamics Note : this cannot be used for studying fluctuations h i T µν (τ, η, x ) LO Higher moments (the connected part only) of the multiplicity distribution in a small slice in rapidity : Moments of the multiplicity distribution are expressible in terms of retarded quantities (FG, Venugopalan) If the p particles in the moment of order p are in the same small slice of rapidity, the locality requirement is satisfied François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 38

43 Quantities that do not factorize For some quantities, an extension of the above form of factorization may be able to resum all the leading logs. Example : 2-gluon correlations with a large rapidity separation between the gluons (work in progress with T. Lappi and R. Venugopalan) More exclusive quantities seem out of reach of this form of factorization : Example : survival probability of rapidity gaps for such quantities, the main obstruction is the impossibility to write them as formulas involving only retarded objects W[ e A ± ] may not contain enough information about the projectiles in order to compute these more detailed observables (W[ e A ± ] is only the diagonal part of the initial density matrix of the incoming nucleus) François Gelis 2008 Workshop on Hot and dense matter in the RHIC-LHC era, TIFR, Mumbai, February p. 39