Neutron Stars By Matthew Buza Star Power l

Neutron Stars By: Matthew Buza

Star Power l l l 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? l l Star Characteristics are given by: l Luminosity l Ave. Mass l Ave. Diameter Which all determines Main Sequence Time. l Ex. The sun is a G 2(spectoral class) and has a main sequence time of 12 billion years.

Stellar Evolution l l l 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.

Nothing Wrong With Second Best l l l 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.

The Touch of God l Supernova l l 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). l l 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.

Neutron Stars l From massive White Dwarf stars to Neutron stars Cooling of the WDS, forms a Fe lattice, with intermittent heavier elements spread throughout. l 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. l l

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

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