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