Cooling of Neutron Stars

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Presentation transcript:

Cooling of Neutron Stars Hovik Grigorian Dubna, JINR Helmholtz International Summer School Dence matter in HIC and Astrophysics Dubna 2008

Cooling of HOT Neutron Stars Lecture 1 Schematic introduction of simulations BOLTZMANN EQUATION IN CURVED SPACE – TIME HEAT TRANSPORT AND NEUTRINO DIFFUSION HOT NEUTRON AND QUARK STAR EVOLUTION QUASI-EQUILIBRATE EVOLUTION OF COMPACT OBJECT Hot COMPACT STARS

Phase Diagram & Cooling Simulations

Cooling of Hybrid Neutron Stars Lecture 2 Configurations of Hybrid stars Cooling processes in QM Crust, SC Gaps and ... Time Evolution of Surface Temperature Constraints from Observations Summary & Discussion

Hybrid Configurations

Cooling Mechanism

Direct URCA in Hadron Matter

DU constraint

HS with different structure

SC pairing gaps

Crust Model

Surface Temperature & Age Data Slow Coolers Intermediate Coolers Fast Coolers

Cooling of light stars Models

C74:025801,2006

The most of pathologies of hadronic stars are descendible Some Anomalies

Why DU is a problem?

Temperature in the Star Interior

Temperature Age – LogN LogS Hybrid Stars Cooling

Cooling of HS with Single flavor QM How to distinguish the different types of Hybrid star models from cooling evolution?

Mass Distribution of NS Could the Mass Distribution of NSs be exstracted from the cooling models?

Extracted Mass Distribution

Summary Cooling of NSs is one of testing schemes for High density matter EoS Mass distribution of NS is extracted from the cooling model Cooling data allowed existence of HS even with one flaver QM DU can be consided as a problem

Open Questions & Discussian Do Hybrid NSs an alternative or the solution of problems of compact stars? Do for all constraints exist a valid HNS model? Can magnetic field and surface heating modify the main conclusions on cooling of NS? Is the mass distribution of NSs an obsorvable?