'Degeneracy pressure' presentation slideshows

ASTR100 (Spring 2008) Introduction to Astronomy Life as a Low-mass Star

ASTR100 (Spring 2008) Introduction to Astronomy Life as a Low-mass Star. Prof. D.C. Richardson Sections 0101-0106. What are the life stages of a low-mass star?. A star remains on the main sequence as long as it can fuse hydrogen into helium in its core. Thought Question.

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Endpoints of stellar evolution

Endpoints of stellar evolution. The end of stellar evolution is an inert core of spent fuel that cannot maintain gas pressure to balance gravity .

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Chapter 18: The Bizarre Stellar Graveyard

Chapter 18: The Bizarre Stellar Graveyard. What is a white dwarf?. White Dwarfs. Sirius B is the closest white dwarf to us. White dwarfs are the remaining cores of dead stars. Electron degeneracy pressure supports them against the crush of gravity. Sirius A + B in X-rays. White Dwarfs.

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Star evolution

Star evolution. Chapters 17 & 18 (Yes, we skip chap. 16, star birth). Goals & Learning Objectives. Learn some simple astronomical terminology Develop a sense of what scientists know about the overall universe, its constituents, and our location Describe stellar evolution

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Life and Evolution of a Massive Star

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Today in Astronomy 102: electron degeneracy pressure and white dwarfs

Today in Astronomy 102: electron degeneracy pressure and white dwarfs. Detailed description of degeneracy pressure: confinement by quantum repulsion (Pauli exclusion principle) leads to additional resistance to compression (wave-particle duality; Heisenberg uncertainty principle).

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Today in Astronomy 102: electron degeneracy pressure and white dwarfs

Today in Astronomy 102: electron degeneracy pressure and white dwarfs. Detailed description of degeneracy pressure: confinement by quantum repulsion (Pauli exclusion principle) leads to additional resistance to compression (wave-particle duality; Heisenberg uncertainty principle).

277 views • 27 slides

Stellar Evolution

Stellar Evolution. Birth Main Sequence Post-Main Sequence Death. Star Birth. Giant Molecular Cloud. 10 3 -10 6 M sun 10-30 K H 2 Very Dense 1-100 lyr across Only GMCs can form stars Gravity must be stronger than pressure. Collapse Triggered. Cloud collapses Cloud becomes lumpy

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Neutral hydrogen in the Galaxy

Neutral hydrogen in the Galaxy. Neutral hydrogen in the Galaxy. HII regions. Orion nebula Triangulum nebula. Interstellar extinction law. Dust in the Eagle nebula. Dust: reddening in colour-colour plot. Calculating E(B-V) from colour-colour plot.

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Lecture 10

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Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9

Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9. Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9. These stages have already been discussed: Stage 1: Interstellar Cloud Stage 2: A Collapsing Cloud Fragment Stage 3: Fragmentation Ceases

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A Solar System Overview

A Solar System Overview. A dynamic solar system; Stellar astronomy; Subatomic particles and nuclear fusion; White dwarfs as end to low mass stars; High mass stellar evolution; Cepheid variables; Supernovae; Neutron stars and black holes. Motivation Not just Astro 2, 5, 10 content...

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Chapter 15: Stellar Graveyard

Chapter 15: Stellar Graveyard. White Dwarfs Neutron Stars Black Holes Gamma-Ray Bursts. 15.1 Degenerate Objects. Objects made of degenerate matter (plasma conditions dominated by degeneracy pressure). White dwarfs are supported by electron degeneracy pressure.

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Star evolution

Star evolution. Chapters 17 & 18 (Yes, we skip chap. 16, star birth). 3 star groups (p. 549). 3 categories of stars: Low mass (<2 M sun ) Intermediate mass (2 ? 8 M sun ) High mass (>8 M sun )

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Lecture 39

Stellar Lives (continued). Galaxies. Last Stages of Low-Mass Stars Lives of High-Mass Stars Galaxies: Types and Structure. Lecture 39. Chapter 17.14 ? 17.16, 18.1 ? 18.5. Last Stages of Evolution. The core helium runs out in ~100 million years.

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