Marcus Bleicher, Frankfurt 2008 Are di-leptons sensitive messengers from the hot and dense stage? Marcus Bleicher Institut für Theoretische.

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Presentation transcript:

Marcus Bleicher, Frankfurt 2008 Are di-leptons sensitive messengers from the hot and dense stage? Marcus Bleicher Institut für Theoretische Physik Goethe Universität Frankfurt Germany

Marcus Bleicher, Frankfurt 2008 Thanks to the UrQMD group Katharina Schmidt Sascha Vogel Xianglei Zhu Daniel Krieg Horst Stoecker Hannah Petersen Ayut Limphirat Stephane Haussler Timo Spielmann Qingfeng Li Special thanks to C. Sturm (HADES)

Marcus Bleicher, Frankfurt 2008 Outline Introduction Baryon densities: methods, results Densities at rho decay Model features Di-leptons Summary

Marcus Bleicher, Frankfurt 2008 Tools: Transport approaches UrQMD, IQMD, HSD, RQMD,… out-of-equilibrium transport model, (rel. Boltzmann equation) Particles interact via : - measured and calculated cross sections - string excitation and fragmentation - formation and decay of resonances - Potentials and in-medium properties Provides full space-time dynamics of heavy-ion collisions

Marcus Bleicher, Frankfurt 2008 Motivation At RHIC: look for signals of freely moving partons. At FAIR/SPS: look for the mixed phase and the onset of deconfinement E. Bratkovskaya, M.B. et al., Phys.Rev.C69:054907,2004

Marcus Bleicher, Frankfurt 2008 Do we understand the interesting stages of the reaction? String matter dominates the early stages (t ~ overlap time) ‘string matter‘ = QGP? H. Petersen, M.B., nucl-th/ However, overall dynamics does not seems to be sensitive to the underlying degrees of freedom I. Arsene et al, nucl-th/ UrQMD, Pb+Pb

Marcus Bleicher, Frankfurt 2008 Phase trajectories I. Arsene et al, nucl-th/

Marcus Bleicher, Frankfurt 2008 What do we want to see?  in-medium spectral functions Mass shift of the  meson roughly from 770 MeV  600 MeV Modified width of the  meson roughly from 150 MeV  300 MeV Possibly modifications of  and   Do we know the densities to the required precission?

Marcus Bleicher, Frankfurt 2008 Problems How are energy density and baryon density defined? (N/V doesn’t work!) - What frame? Landau? Eckardt? - Lorentz contraction? Nucleus? Nucleon? Is the system thermalized? - Viscous contributions in hydro? What are the degrees of freedom?

Marcus Bleicher, Frankfurt 2008 Baryon density Define baryon density at point r in the Eckardt frame (vanishing baryon flow)  I.e.   (r)  j 0 B (r) in the frame with j  =(   0) Lorentz contraction for the nucleons along the beam axis is taken into account

Marcus Bleicher, Frankfurt 2008 Further problem: thermalization Sound definition of the baryon current/density is possible However, free streaming effects are not excluded (the defined baryon density is not necessarily thermal)  consider only particles that have a velocity around to the thermal velocity (similar to three- fluid approach, Brachmann et al) not practical for transport…

Marcus Bleicher, Frankfurt 2008 Local baryon densities (Averaged over the positions of all hadrons) Are we able to observe unambiguous signals from the most compressed region of the system? Central Au+Au/Pb+Pb collisions

Marcus Bleicher, Frankfurt 2008 Baryon densities in momentum space at the point of the rho decay (GeV) Central Au+Au/Pb+Pb reactions

Marcus Bleicher, Frankfurt 2008 Gain and loss rates of rho mesons Maximal densities reached at t=10,4,2 fm rho production at HADES energies driven by baryon resonance decays at higher energies: major early stage production, but still sizeable tail from decays in the late stage

Marcus Bleicher, Frankfurt 2008 Absorption vs decay How are the dileptons calculated? Shining vs decay Strong absorption in the early stages

Marcus Bleicher, Frankfurt 2008 Density distributions Distribution baryon density at the point of rho decay or absorption Significantly higher reach in density if absorbed rhos are included. (However, here the integrated rho life times are shorter)

Marcus Bleicher, Frankfurt 2008 Density vs rho mass Absorption has the highest reach in density  shining method necessary? Moderate mass dependence Final feeding from decays around 1-2 ground state density M (GeV)

Marcus Bleicher, Frankfurt 2008 Difference between shining and other approaches Thin lines: ‘no absorption’ Blue lines: only final decays Green lines: ‘shining’

Marcus Bleicher, Frankfurt 2008 Are the dynamical models good enough? Check space-time evolution  HBT correlations Check particle production  Pion production (    !)  Baryon resonances (  from decays !)  Final state  from  correlations

Marcus Bleicher, Frankfurt 2008 Excitation functions  Good agreement between different transport models (HSD/UrQMD)  4 pi and midrapidity abundancies are described on a 10-20% level (systematic error)  Energy dependence: OK  Hadron-string models work well E. L. Bratkovskaya, M.B., et al, Phys. Rev. C 69, (2004)

Marcus Bleicher, Frankfurt 2008 Detailed view at low energies Comparison to KAOS data Reasonable agreement CC   + UrQMD Au+Au   + UrQMD D. Schumacher, H. Petersen D. Schumacher, s. Vogel, M.B, Acta Phys.Hung.A27: ,2006

Marcus Bleicher, Frankfurt 2008 HBT-Energy dependence Data shows no dramatic features Expansion and decoupling dynamics ok Fireball life time ok UrQMD

Marcus Bleicher, Frankfurt 2008 Why resonances are interesting? There is a (long living) hadronic rescattering stage at FAIR and SPS energies Lifetime and properties of the hadronic stage are defined and probed by resonance production/absorption/re-feeding/decay Use different resonances to explore this stage: e.g. mesons: baryons: Are resonances dissolved/broadened/shifted in matter?

Marcus Bleicher, Frankfurt 2008 The rho has additional potential: Hadronic vs leptonic channel 00 0 -- ++ 00 - + 00 00 -- ++ ++ -- Hot and dense medium A+A Particle yields Particle spectra time L* p K p p K

Marcus Bleicher, Frankfurt 2008 Decay time distribution of  mesons Resonance formation needs time (most  from baryon resonances)  even short lived resonances are dominantly from later stages

Marcus Bleicher, Frankfurt 2008 Expected multiplicities Pion reconstruction is free from   e+e- model UrQMD S. Vogel, M. Bleicher, Phys.Rev.C74:014902,2006

Marcus Bleicher, Frankfurt 2008 Di-leptons: Some technical issues Different di-lepton physics: - VMD, EVMD, form factors, - collisional broadening, shining, - explicit ,  effective , instant di-leptons  Different result from same input!  Standard / consensus needed Bremsstrahlung?!

Marcus Bleicher, Frankfurt 2008 Hadrons  di-leptons

Marcus Bleicher, Frankfurt 2008 Comparison to 160 AGeV CERES Data from 2000 UrQMD (Pb+Au) is filtered D. Schumacher, M.B. Well known dip around 500 MeV Dip is from low momentum di-lepton pairs

Marcus Bleicher, Frankfurt 2008 FAIR energy: UrQMD Strong contribution from  resonances Rather broad structure from the  meson

Marcus Bleicher, Frankfurt 2008 HADES energies: UrQMD Note the broad  mass distribution D. Schumacher, s. Vogel, M.B, Acta Phys.Hung.A27: ,2006

Marcus Bleicher, Frankfurt 2008 Trivial rho broadening Coupling to baryon resonances broadens the rho meson mass distribution even without ‘explicit’ medium contribution Schumacher, Vogel, Bleicher, Acta Phys.Hung.A27: ,2006

Marcus Bleicher, Frankfurt 2008 HADES energies: IQMD/RQMD IQMD, (instant di-leptons: no baryon- and  resonance propagation) RQMD, (effective , no  and  propagation) Phys.Lett.B640: ,2006 nucl-th/

Marcus Bleicher, Frankfurt 2008 Di-lepton summary Model differences due to different di-lepton ‘after burner’! Clear hint of non-equilibrium contributions HADES, nucl-ex/

Marcus Bleicher, Frankfurt 2008 Summary  Theory has to get space-time structure and particle densities right (di-leptons are integrated over fireball lifetime and sensitive to baryon res. and  collisions)  Fundamentals, e.g. definition of densities (frames, methods, thermal fraction) have to be fixed  Bremsstrahlung might be important for 1-2 AGeV reactions, however double counting needs to be avoided  The underlying transport models are mostly consistent with each other, however di-lepton after burners are not  Real  vs. effective  vs. instant leptons  Standard‘ model for hadron to di-lepton conversion needed