Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek 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 Phase Diagram & Cooling Simulations Structure and stability of NS DU constraint Hybrid Configurations HS with different structure Cooling Mechanism SC pairing gaps Crust Model Surface Temperature & Age Data Cooling of light stars Models Some Anomalies The most of pathologies of hadronic stars are descendible Patalogies of hadronic stars are descendible 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? 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?