'Hydrostatic equilibrium' presentation slideshows

Topic E: Astrophysics

Topic E: Astrophysics. The following notes were taken primarily from Physics for IB by Chris Hamper and Physics Course Companion by Tim Kirk. Are they real?. E.1.1 Outline the general structure of the solar system.

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The Solar System

940 views • 69 slides

Objectives

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MAIN SEQUENCE STARS, Red Giants and White Dwarfs

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PRIN 2001: Summary of the activities of the Research Unit at the

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Dwarf Planets

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The Sun, Our Star

The Sun, Our Star. Arny, 3 rd Edition, Chapter 11. Introduction. Introducing the Sun The Sun is a star, a luminous ball of gas with a radius more than 100 times and a mass more than 300,000 times bigger than the Earth

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Stars form from condensing clouds of gas & dust

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Open Clusters

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PH507 The Hydrostatic Equilibrium Equations for Stars

PH507 The Hydrostatic Equilibrium Equations for Stars. Dr J. Miao. We will cover the following topics:. Equation of Mass distribution Equation of hydrostatic support - Virial Theorem -Centre pressure and mean temperature of a star -Different time scales for stars

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Novae and Mixing

Novae and Mixing. John ZuHone ASCI/Alliances Center for Thermonuclear Flashes University of Chicago. Overview. Purpose What is FLASH? Mixing in Novae Setting Up the Problem Doing the Problem Conclusions. Purpose.

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From temporal spectra to stellar interiors (and back)

342 views • 22 slides

Star Formation

0. Star Formation. 0. Giant Molecular Clouds. Barnard 68. Infrared. Visible. Star formation ? collapse of the cores of giant molecular clouds : Dark, cold, dense clouds obscuring the light of stars behind them . 0. Parameters of Giant Molecular Clouds. Size: r ~ 50 pc.

655 views • 19 slides

Star Formation

0. Star Formation. 0. Giant Molecular Clouds. Barnard 68. Infrared. Visible. Star formation ? collapse of the cores of giant molecular clouds : Dark, cold, dense clouds obscuring the light of stars behind them . 0. Parameters of Giant Molecular Clouds. Size: r ~ 50 pc.

338 views • 19 slides

Stellar Structure

Stellar Structure. Chapter 10. From this, can we infer the internal structure?. Stellar Structure. We know external properties of a star L, M, R, T eff , (X,Y,Z). Apply basic physical principles. P + dP pressure on top of cylinder, P on bottom

538 views • 19 slides

Today

Today. Hand in any work needed. Get out a small piece of paper, PUT YOUR NAME ON IT. When bell rings the quiz will start and you will have 1 minute per question to answer. Question 1. What are the dark spots on the moon called?. Question 2.

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Lecture 12

Lecture 12. Stellar structure equations. Convection. A bubble of gas that is lower density than its surroundings will rise buoyantly

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Section 5.4 Gravity Waves

Section 5.4 Gravity Waves. Gravity Waves. Gravity acts as the restoring force on parcels displaced from hydrostatic equilibrium. Pure gravity exists when the fluid is stably stratified. Two types of gravity waves:

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The Bullet Cluster: cases for Dark Matter and MOND

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Life Cycle of Stars

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