'Massive stars' diaporamas de présentation

This Is Your Life

This Is Your Life. But first, a little background. Kirchhoff's Laws. Kirchhoff's laws ,there are three types of spectra: continuum, emission line, and absorption line. . High pressure, high temperature gas. Low pressure, high temperature gas. Cool gas in front of continuous spectra source.

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Prentice Hall EARTH SCIENCE

Prentice Hall EARTH SCIENCE. Tarbuck Lutgens . ?. Chapter 25. Beyond Our Solar System. Characteristics of Stars. 25.1 Properties of Stars . A constellation is an apparent group of stars originally named for mythical characters. The sky contains 88 constellations.

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Earth Science 25.2A : Stellar Evolution

Earth Science 25.2A : Stellar Evolution . The Birth and Evolution of Stars . Earth Science 25.2 : Stellar Evolution . Determining how stars are born, age and die can be difficult because the life of a star can span billions of years.

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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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HST observations of three GHRs in M101

HST observations of three GHRs in M101. Rosie Chen et al. arXiv:astro-ph/0410240 Reporter: Feng Li. Outline. Introduction Observations Methods Clusters in three GHRs Discussion. Introduction. GHRs: Giant HII Regions sites of star and cluster formation.

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STARS

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Massive Stars as the Progenitors of (long) Gamma-Ray Bursts

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The Deaths of Stars

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Habitable Zone

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Faint Supernova or Super-AGB star?: SN 2008S in context

Faint Supernova or Super-AGB star?: SN 2008S in context. Margaret Meixner STScI Masaaki Otsuka STScI/ASIAA David Riebel JHU SEEDS consortium. SN2008S: Spitzer IRAC 3.6 micron. Day 17. Day 180. Wesson et al. (2009).

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Get out your journals

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Chapter 20 part 2:

Chapter 20 part 2:. Star death: 0.4 - 4 M ? Carbon White dwarfs > 4 M ? Supernova SN1987A Neutrinos Supernovae involving white dwarfs Supernova remnants. Massive stars. Supergiants. Massive stars. Core-collapse supernova. Turbulence. Turbulence. Observing supernovae.

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The Galactic Centre: a hidden treasure

The Galactic Centre: a hidden treasure. How can we study the Galactic centre? What is do we find there? What does it tell us about our Galaxy, and galaxies in general?. Galactic Bulges. Classic view of spiral galaxies young stars in spiral arms old stars in halo and bulge

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Epoch of Reionization

Epoch of Reionization. History of Hydrogen. z > 1000: hot universe, hydrogen is ionized, universe is opaque to radiation z = 1000: hydrogen recombines, becomes transparent to radiation, CMB decouples from matter

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Supernovae as neutrino and gravitational wave sources

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Quiz 3

Quiz 3. Briefly explain how a low-mass star becomes hot enough to settle on the main-sequence. Describe what is solar weather and list two ways in which it can affect Earth. What are Cepheid variables and WD supernovae, and why they are important in astronomy?

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To Do

To Do. Take out 2 sheets of paper for notes Ch. 15-2 (part 3) | Types of Stars Ch. 15-3 | Galaxies. 15-2 (Part 3) | The Life Cycle of Stars. The Aging of Massive Stars. Massive stars use their hydrogen much faster than stars like the sun do

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Asteroid Close Approaches

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Stars and Their Spectrums

Stars and Their Spectrums. Stars are the Element Factories of the Universe. Stars fuse _________ into _________most of their lives. Stars fuse hydrogen into helium most of their lives. Younger stars are rich in hydrogen. Older stars are rich in helium.

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