DOC PREVIEW
IUPUI AST 105 - Stars

This preview shows page 1 out of 3 pages.

Save
View full document
View full document
Premium Document
Do you want full access? Go Premium and unlock all 3 pages.
Access to all documents
Download any document
Ad free experience
Premium Document
Do you want full access? Go Premium and unlock all 3 pages.
Access to all documents
Download any document
Ad free experience

Unformatted text preview:

Ast 105 1nd Edition Lecture 12 Outline of Last Lecture (#12)I. Giantsa. 6 steps to form II. Helium Fusiona. Helium flashIII. Variable Starsa. Instability strip b. Low-mass starsc. High-mass starsd. Ceiphadse.Outline of Current Lecture (#13)I. Death of starsII. AGB starsIII. White DwarfIV. Electron Degeneracy PressureV. Chandra Sakhar VI. NovaVII. Roche LimitVIII. Low and High Mass stars Current LectureDeath of Stars- Is dependent on the main sequence mass- low mass stars < 8 Msun Low Mass Stars- The max temperature is only 200 million Kelvin, therefore no fusion of carbon or oxygen- As the helium fusion in the court begins to slow down, photon production drops off Gravity begins to dominate and enter regions again contract This heats up the shell of helium just above the core, thus shellhelium fusion begins- Just above this we have hydrogen shell fusion- The helium fusion in the shell pushes the outer regions of the star to larger radii, this forms an aymptonic giant branch star (AGB Star)- At the end of AGB, Helium shell flashes occur (more than once) This causes the outer layers to expand and thus cool, and the electrons combined with ions to form atoms  this produces more photons Helium shell flashes and recombination photons a large production of protons- thus (outermost regions) materials ejected is called “planetary nebula”- As the outer regions are blessed away, the hot interior region of the star is exposed the star moves leftward on the H2 diagram (inner regions are at a much higher temp.White Dwarf- As outer layers of both the way, the high temp carbon oxygen core is exposed.This forms a white dwarf- White dwarfs are stable.  The gravity is balanced by electron degeneracy pressureElectron Degeneracy Pressure - The carbon and oxygen are ionized.  Electrons are separated from the nuclei- Nuclei are squeezed into a crystalline arrangement- Electrons distributed around crystals, but are very close to each other- Electrons do not like to be next to each other Pauli Exclusion Principle- As gravity tries to force electrons together, many of them vibrate faster and faster so that the quantum numbers are not identical  This vibration of electrons pushes against the contraction forces of gravityChandraSekhar - In 1940, he found that as long as the mass of the white dwarf was less then 1.4 Msun, the electron degernacy pressuer could balance gravity - limit: white dwarf masses are less than 1.4Msun - Our son will end up as a white board. - 1 teaspoon of white dwarf ways five timesNova In binary systems with a main sequence and white wharf, main sequence Is within the Roche limit of the white wharf, the hydrogen is pulled off the main sequence and onto the white dwarfhydrogen fusion explosion Nova Roche Limit Gravity of a white dwarf is greater than the self-gravity of main sequenceHigh Mass Star- >8 Msun- Here, gravity is sufficient to collapse the core after hearing infusion and drivethe temperature to over 600 million K- For the larger stars, temps get even higher.  This is how almost all of the elements are made- The large number of fusion generated photons created in shells pushes the outer layers far awaythis forms a


View Full Document

IUPUI AST 105 - Stars

Download Stars
Our administrator received your request to download this document. We will send you the file to your email shortly.
Loading Unlocking...
Login

Join to view Stars and access 3M+ class-specific study document.

or
We will never post anything without your permission.
Don't have an account?
Sign Up

Join to view Stars 2 2 and access 3M+ class-specific study document.

or

By creating an account you agree to our Privacy Policy and Terms Of Use

Already a member?