Cooling of Neutron Stars

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Cooling of Neutron Stars

• Hovik Grigorian
• Dubna, JINR

Helmholtz International Summer School Dence
matter in HIC and Astrophysics
Dubna 2008
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Cooling of HOT Neutron StarsLecture 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

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Phase Diagram Cooling Simulations
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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

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Hybrid Configurations
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Cooling Mechanism
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Direct URCA in Hadron Matter
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DU constraint
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HS with different structure
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SC pairing gaps
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Crust Model
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Surface Temperature Age Data
Slow Coolers
Intermediate Coolers
Fast Coolers
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Cooling of light stars Models
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C74025801,2006
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Some Anomalies
The most of pathologies of hadronic stars are
descendible
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Why DU is a problem?
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Temperature in the Star Interior
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Temperature Age LogN LogSHybrid Stars Cooling
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Cooling of HS with Single flavor QM

• How to distinguish the different types of Hybrid
  star models from cooling evolution?

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

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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?