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

2. 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

3. Phase Diagram & Cooling Simulations

18. 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

21. Hybrid Configurations

22. Cooling Mechanism

23. Direct URCA in Hadron Matter

24. DU constraint

25. HS with different structure

26. SC pairing gaps

27. Crust Model

28. Surface Temperature & Age Data
Slow Coolers
Intermediate Coolers
Fast Coolers

29. Cooling of light stars Models

30. C74:025801,2006

31. The most of pathologies of hadronic stars are descendible
Some Anomalies

32. Why DU is a problem?

33. Temperature in the Star Interior

34. Temperature Age – LogN LogS Hybrid Stars Cooling

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

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

37. Extracted Mass Distribution

38. 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

39. 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?