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http://hdl.handle.net/10761/989

Data:  14feb2012 
Autori:  Jaccarino, Danilo 
Titolo:  A complete calculation of Shear Viscosity in Strongly Interacting matter 
Abstract:  The last observations from the Heavy Ion Collider facilities keep marking new territories in the unexplored field of the high temperature T QuarkGluon Plasma, with new discoveries that seem to enforce the hypothesis that such an exotic state of Strongly Interacting matter can indeed exist, making it an established fact. Things in the finite baryon density opposite regime are much harder as QCD, and its Lattice formulation, cannot yield any quantitative prediction to date, due to the strongcolour confinement effects in matter at high densities. Nevertheless its behaviour can be inferred from the empirical observations of Neutron Stars, that are sensitive to the composition, and thermodynamical properties of the Nuclear Matter Equation of State.
This thesis is focused on the construction of a Hybrid Equation of State, imposing a FirstOrder colour deconfinement transition of the Second Kind  as pointed out by Lattice QCD studies  between the two phases. Nuclear Matter is described by means of the microscopic BruecknerHartree Fock Many Body theory, that builds the in medio properties of interacting nucleons starting from the consistent treatment of realistic Bonn B 2body vacuum interactions plus effective 3body forces; Quark Matter is instead treated as a free gas of massless u,d,s quarks with the MIT Bag Model. Shear Viscosity of the strongly interacting Fermi liquid is then calculated in a lowtemperature BoltzmannLandau transport approach, yielding a slight deviation from the AbrikosovKhalatnikov standard result at quark degrees of freedom dominated densities. The calculations are finally applied to the Astrophysics of Compact Objects: Neutron Stars static configurations are evaluated by means of the relativistic "TolmanOppenheimerVolkoff" structure equations, finding a upper mass limit of 1.81 Solar Masses for the Hybrid Equation of State; furthermore, the estimate of the damping timescales of rotational rmode Oscillations in Neutron Stars, sensitive to both the Equation of State and to Shear Viscosity of Hybrid Matter, are performed and confronted with the typical Gravitational Radiation instability timescales: the latter dominate in young, cooling Neutron Stars and this could be a promising signal for the LIGO facility, while in old Neutron Stars, at T=0.00001 MeV, the l=m=2 rotationalmode is alone able to suppress the GW emission.
Despite the title, the calculation is far from being "complete", but it describes many features in a consistent way supported from the solidity of microscopic calculations of the Strongly Interacting matter properties. 
In  Area 02  Scienze fisiche

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