Post on 08-Feb-2021
Quark matter deep inside compact starsDavid Blaschke (University of Wroclaw, Poland & JINR Dubna, Russia)
PSR J16142230PSR J0348+0432
Antoniadis et al., Science 340 (2013) 448 Demorest et al., Nature 467 (2010) 1081
Helmholtz International Summer School, Dubna, 25.07.14“Nuclear Theory and Astrophysical Applications”
Coloured condensates (CC) Deep inside compact stars?
● Cooper instability● Quark condensates● Symmetries and pairing patterns● Twoflavor color superconductors 2SC phase→● Threeflavor color superconductors CFL phase →● NJL model and NambuGorkov formalism● Mean field gap equations and solutions● Thermodynamic potential● Phase diagram● EoS and TOV equations – Hybrid stars with CC
Cooper instabilities
Cooper instabilities
Field operators
Quarkantiquark condensates
Diquark condensates
Diquark condensates
Operators in flavor and color space
Operators in Dirac space
Combined operators
Twoflavor color superconductors
Symmetry properties: color
Symmetry properties: global symmetries
Threeflavor color superconductors
Threeflavor color superconductors
Pairing patterns
Colorflavor locking
NJL model for color superconductivity
NambuGorkov formalism
NambuGorkov propagator
Selfconsistency problem
Gap equation
Propagator
Dispersion relations
Dispersion relations (CFL)
Gap equation: solutions
Gap equation: solutions
Gap equation: solutions
Thermodynamic potential
Thermodynamic potential
Thermodynamic quantities
Minima
Condensation energy
CFL pairing in the bag model
Realistic masses
Realistic masses
Which phase is favored ?
Which phase is favored ?
3flavor NJL model
Results for T=0
Phase diagram
S. Ruester et al. Phys. Rev. D 72 (2005) 034004D. Blaschke et al. Phys. Rev. D 72 (2005) 065020
Quark matter in compact stars
Modern topics (selected): Hyperon puzzle (M. Baldo et al.; P. Haensel at al..; ...) Direct Urca problem (T. Klaehn et al.) Supernova explosion mechanism (T. Fischer et al.)
Solutions can be provided by Stiffening of hadronic matter by quark substructure effects (Pauli blocking excluded volume)→ Stiffening of quark matter at high densities (e.g., by multiquark interactions) Resulting early onset of quark matter and large latent heat
Crosstalk with HeavyIon Collision Experiments
Hyperon puzzle & quark matter
Massradius sequences for different model equations of state (EoS) illustrate how the three major problems in the theory of exotic matter in compact stars (left panel) can be solved (right panel) by taking into account the baryon size effect within a excluded volume approximation (EVA). Due to the EVA both, the nucleonic (NEVA) and hyperonic (BEVA) EoS get sufficiently stiffened to describe highmass pulsars so that the hyperon puzzle gets solved which implies a removal of the reconfinement problem. Since the EVA does not apply to the quark matter EoS it shall be always sufficiently different from the hadronic one so that the masquerade problem is solved.
Exploring hybrid star matter at NICAT.Klähn (1), D.Blaschke (1,2), F.Weber (3)(1) Institute for Theoretical Physics, University of Wroclaw, Poland
(2) Joint Institute for Nuclear Research, Dubna(3) Department of Physics, San Diego State University, USA
HeavyIon Collisions Compact Stars
„The CBM Physics Book“, Springer LNP 841 (2011), pp.158181NICA White Paper, http://theor.jinr.ru BLTP TWikipages →
Proposal: 1. Measure transverse and elliptic flow for a wide range of energies (densities) at NICA and perform Danielewicz's flow data analysis > constrain stiffness of high density EoS2. Provide lower bound for onset of mixed phase > constrain QM onset in hybrid stars
stiff EoS(at flow limit)
low ncrit(at NICA fixT)
soft EoS (dashed line)
high Mmax(J16142230)
low Monset (all NS hybrid)
excluded(J16142230)
http://theor.jinr.ru/
Quark matter in 2Msun neutron stars? → only color superconducting + vector int.
T. Klahn et al., PRD 88 (2013) 085001; arxiv:1307.696
Baryon substructure effect (EVA)
Thermodynamic consistency:
Parametrization of excluded volume with nonlinear dependence on the chemical potential:
NJL model with multiquark interactions
Meanfield approximation:
Thermodynamic Potential:
Result:
Hybrid EoS supports MR sequences with highmass twin compact stars
S. Benic, D. Blaschke, D. AlvarezCastillo, T. Fischer, in progress (2014)
28 membercountries
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Kickoff: Brussels, November 25, 2013
by July 26, 2013:
MP1304
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