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| - | === Formation of Neutron Stars === | + | ==== Formation of Neutron Stars ==== |
| Neutron stars can arise from supernova explosions of massive stars (between ~8 and 30 solar masses), from the merger of white dwarfs, or from the merger of light neutron stars. | Neutron stars can arise from supernova explosions of massive stars (between ~8 and 30 solar masses), from the merger of white dwarfs, or from the merger of light neutron stars. | ||
| - | === Internal Structure of Neutron Stars=== | + | ==== Internal Structure of Neutron Stars==== |
| Because of their extremely high densities, neutron stars are a perfect nuclear physics laboratory. Hence, measuring neutron star properties allows us to place constraints on the matter at supranuclear densities. Given that such densities are not reachable on Earth, we rely on theoretical models describing the neutron star interior, but those come with large uncertainties. | Because of their extremely high densities, neutron stars are a perfect nuclear physics laboratory. Hence, measuring neutron star properties allows us to place constraints on the matter at supranuclear densities. Given that such densities are not reachable on Earth, we rely on theoretical models describing the neutron star interior, but those come with large uncertainties. | ||
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| The following figure (from Dany Page). | The following figure (from Dany Page). | ||
| - | {{NS_structure.jpg|Neutron Star Structure}} | + | {{ns_structure.jpeg|Neutron Star Structure}} |
Last modified: le 2022/07/18 08:52
