cooling of hybrid neutron stars hovik grigorian yerevan state university dubna, jinr ladek zdroj2008

Cooling of Hybrid Neutron Stars

Hovik GrigorianYerevan State University

Dubna, JINR

Ladek Zdroj2008

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

Patalogies of hadronic stars are descendible

The most of pathologies of hadronic stars are descendible

Why DU is a problem?

Temperature in the Star Interior

Temperature Age – LogN LogSHybrid 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?