Lecture 22

Lecture 22 - Today (Mon.) in Today (Mon.) in Astro Astro 3...

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Unformatted text preview: Today (Mon.) in Today (Mon.) in Astro Astro 3 3 Cell phones on vibrate now, please The Plan: Online quiz 8 due TUESDAY 11 p.m. Today: Chapter 13 Neutron stars and black holes Office hrs. 2:30-4 Units of Chapter 13 9 Neutron Stars 9 Pulsars 9 Neutron Star Binaries 9 Gamma-Ray Bursts Black Holes Einsteins Theories of Relativity Space Travel Near Black Holes Observational Evidence for Black Holes 12.4 Evolution of Stars More Massive than the Sun 13.1 Neutron Stars After a Type II supernova , part of the core may survive as a neutron star. It is as dense as an atomic nucleus. Billions of tons per teaspoonful. Neutron stars have 1-3 solar masses, but are very small, about 10 km in diameter . (A white dwarf is about the size of Earth.) Tremendous pressure of the core collapse: electrons combine with protons, making neutrons and neutrinos Neutrons collapse to the center, forming a neutron star This takes a fraction of a second! 13.1 Neutron Stars Rotation as the parent star collapses, the neutron core spins very rapidly, conserving angular momentum. Typical periods are fractions of a second. Magnetic field as a result of the collapse, the neutron stars magnetic field becomes enormously strong. Pulsar (1967): a radio source flashing regularly: 13.4 Gamma-Ray Bursts amma-ray bursts (much higher energy than X-rays) ound by military satellites....
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Lecture 22 - Today (Mon.) in Today (Mon.) in Astro Astro 3...

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