cooling of hybrid neutron stars hovik grigorian yerevan state university dubna, jinr ladek zdroj2008
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![Page 1: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/1.jpg)
Cooling of Hybrid Neutron Stars
Hovik GrigorianYerevan State University
Dubna, JINR
Ladek Zdroj2008
![Page 2: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/2.jpg)
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
![Page 3: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/3.jpg)
Phase Diagram & Cooling Simulations
![Page 4: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/4.jpg)
Structure and stability of NS
![Page 5: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/5.jpg)
DU constraint
![Page 6: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/6.jpg)
Hybrid Configurations
![Page 7: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/7.jpg)
HS with different structure
![Page 8: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/8.jpg)
Cooling Mechanism
![Page 9: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/9.jpg)
SC pairing gaps
![Page 10: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/10.jpg)
Crust Model
![Page 11: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/11.jpg)
Surface Temperature & Age Data
![Page 12: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/12.jpg)
Cooling of light stars Models
![Page 13: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/13.jpg)
Some Anomalies
Patalogies of hadronic stars are descendible
The most of pathologies of hadronic stars are descendible
![Page 14: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/14.jpg)
Why DU is a problem?
![Page 15: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/15.jpg)
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?
![Page 18: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/18.jpg)
Could the Mass Distribution of NSs be exstracted from the cooling models?
![Page 19: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/19.jpg)
Extracted Mass Distribution
![Page 20: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/20.jpg)
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
![Page 21: Cooling of Hybrid Neutron Stars Hovik Grigorian Yerevan State University Dubna, JINR Ladek Zdroj2008](https://reader037.vdocuments.site/reader037/viewer/2022102808/56649d3f5503460f94a181ba/html5/thumbnails/21.jpg)
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?