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Neutron Stars

Neutron Stars. By: Matthew Buza. Star Power. Importance of Stars and their role in the universe. Overview of all stars, and basic characteristics. Stellar Evolution: Start  finish Path to a Neutron Star. Further work being done. Stars?. Star Characteristics are given by: Luminosity

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Neutron Stars

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  1. Neutron Stars By: Matthew Buza

  2. Star Power • Importance of Stars and their role in the universe. • Overview of all stars, and basic characteristics. • Stellar Evolution: Start  finish • Path to a Neutron Star. • Further work being done.

  3. Stars? • Star Characteristics are given by: • Luminosity • Ave. Mass • Ave. Diameter • Which all determines Main Sequence Time. • Ex. The sun is a G2(spectoral class) and has a main sequence time of 12 billion years.

  4. Stellar Evolution • Laws same here as they are on other planets, stars, universe. • Gravity is the same thing that keeps you on the ground, and the earth going around the sun. • We are chemically the same material as planets, stars. • Important to understand the world around us. • Exploring here on earth workings of stars we understand better the cosmos and ourselves. • Understand the basic principles that govern our world and us.

  5. Nothing Wrong With Second Best • Not just the stars we should study, but the by products of them. • Basically, we are looking at the competition of Gravity vs. everything else( kinetic effects, nuclear forces, degeneracy's, electro-magnetic) • Normal stars are fighting with Hydrodynamic pressure, and radiation pressure. • But in by-products we see both electron and neutron degeneracy’s, along with neutrino pressures. Where density is the dominating factor. • Mainly, White Dwarfs, Neutron Stars, and Black holes.

  6. The Touch of God • Supernova • Star begins to fuse iron, which eats up energy. • Causes the star to contract, gravity taking over • Varying densities causes pressure build up, and then the ‘bounce’ (degenerate core), the star violently ejects large amounts of the star into space. • Small Stellar objects are left behind, depending on the core that is left (mass). • This dictates the finally product, governed by the Chandrasekar limit (1.44 sol) , which is the maximum mass of a white dwarf star. • Neutron Stars are generally 1.4-3 solar masses.

  7. Neutron Stars • From massive White Dwarf stars to Neutron stars • Cooling of the WDS, forms a Fe lattice, with intermittent heavier elements spread throughout. • Supported by Electron degeneracy, has a completely free degenerate electron gas • If Fermi energy exceeds the Neutron-Proton mass difference, new exothermic reaction occurs, Reverse Beta-Decay • e + p  n + ve • Supported by Neutron Degeneracy.

  8. Neutron Stars • From White Dwarf star to Neutron star • Density from 1000 tons per cubic inch to 10 billion tons per cubic inch. • From 10,000 miles in diameter to about 10 miles.

  9. What is being worked on? • ‘Pasta’ simulations here at FSU. • Studying multiple densities, running simulations and looking for ‘clumping’ of the protons. • Exploring these characteristics could help to describe many of the characteristics of the neutron stars • Surface features, starquakes, spinning up or down of the star (pulsars). • We hope that this could open up some explanation for why things happen.

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