1. Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008

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

3. Phase Diagram & Cooling Simulations

4. Structure and stability of NS

5. DU constraint

6. Hybrid Configurations

7. HS with different structure

8. Cooling Mechanism

9. SC pairing gaps

10. Crust Model

11. Surface Temperature & Age Data

12. Cooling of light stars Models

13. Some Anomalies Patalogies of hadronic stars are descendible The most of pathologies of hadronic stars are descendible

14. Why DU is a problem?

15. Temperature in the Star Interior

16. Temperature Age – LogN LogS Hybrid Stars Cooling

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

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

19. Extracted Mass Distribution

20. 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

21. 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?