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Astronomy · L5 · Neutron Star Structure, the TOV Equation, and Pulsars/Magnetars · flowchart

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by @openstemUpdated Astronomy
Core collapseelectron capturep + e⁻ → n + ν_eNeutron degeneracy pressurehalts collapseHot proto-neutron star(cools via neutrino emission, ~10 s)Rotation andmagnetic field strength?Radio pulsarlighthouse beam, spin-downMagnetarSGR / AXP, giant flaresSpin-down via magneticdipole radiation + windB ~ 10⁷–10⁹ T, rotation-poweredB ~ 10¹⁰–10¹¹ T, field-powered

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