cooling of neutron stars
DESCRIPTION
Cooling of Neutron Stars. Hovik Grigorian Dubna, JINR. Helmholtz International Summer School Dence matter in HIC and Astrophysics. Dubna 2008. Cooling of H OT Neutron Stars Lecture 1. Schematic introduction of simulations BOLTZMANN EQUATION IN CURVED SPACE – TIME - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/1.jpg)
Hovik GrigorianDubna, JINR
Dubna 2008Helmholtz International Summer SchoolDence matter in HIC and Astrophysics
![Page 2: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/2.jpg)
• 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
![Page 3: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/3.jpg)
![Page 4: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/4.jpg)
![Page 5: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/5.jpg)
![Page 6: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/6.jpg)
![Page 7: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/7.jpg)
![Page 8: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/8.jpg)
![Page 9: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/9.jpg)
![Page 10: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/10.jpg)
![Page 11: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/11.jpg)
![Page 12: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/12.jpg)
![Page 13: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/13.jpg)
![Page 14: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/14.jpg)
![Page 15: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/15.jpg)
![Page 16: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/16.jpg)
![Page 17: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/17.jpg)
![Page 18: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/18.jpg)
Configurations of Hybrid stars Cooling processes in QM Crust, SC Gaps and ... Time Evolution of Surface Temperature Constraints from Observations Summary & Discussion
![Page 19: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/19.jpg)
![Page 20: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/20.jpg)
![Page 21: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/21.jpg)
![Page 22: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/22.jpg)
![Page 23: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/23.jpg)
![Page 24: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/24.jpg)
![Page 25: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/25.jpg)
![Page 26: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/26.jpg)
![Page 27: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/27.jpg)
![Page 28: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/28.jpg)
![Page 29: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/29.jpg)
![Page 30: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/30.jpg)
C74:025801,2006
![Page 31: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/31.jpg)
The most of pathologies of hadronic stars are descendible
![Page 32: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/32.jpg)
![Page 33: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/33.jpg)
![Page 34: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/34.jpg)
![Page 35: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/35.jpg)
How to distinguish the different types of Hybrid star models from cooling evolution?
![Page 36: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/36.jpg)
Could the Mass Distribution of NSs be exstracted from the cooling models?
![Page 37: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/37.jpg)
![Page 38: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/38.jpg)
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 39: Cooling of Neutron Stars](https://reader037.vdocument.in/reader037/viewer/2022102819/5681458c550346895db2758b/html5/thumbnails/39.jpg)
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?