'Main sequence stars' presentation slideshows

To the Stars and Beyond

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Stellar Evolution Review

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Stars

Stars. Dr Katy Lancaster. Overview. Introduction to stars What they are What we can measure The Hertzsprung-Russell Diagram Star life cycles Evolution of stars across the HR diagram. The Sun and all the stars we can see at night are part of the Milky Way galaxy.

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The life history of a star depends primarily on its mass A little bit on its metallicity ( Z )

Stellar Evolution. Stars form from cool clouds of gas called molecular clouds Gravity overcomes pressure, and several stars begin to form Usually get multiple stars in the same region, about the same age Called clusters Initially, the stars are all moving together at the same speed

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Lecture 18

Lecture 18. Stellar populations. Stellar clusters. S imple stellar populations: stars were probably all born at nearly the same time; thus have the same age and composition. Open clusters: contain 10-1000 stars loose structure. Globular clusters: 1000 - 1 million stars

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Stellar Evolution

Chapter 12 Clickers. Stellar Evolution. Question 1. Stars like our Sun will end their lives as. a) red giants. b) pulsars. c) black holes. d) white dwarfs. e) red dwarfs. Question 1. Stars like our Sun will end their lives as. a) red giants. b) pulsars. c) black holes.

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Review

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The power plant of the Sun and stars

The power plant of the Sun and stars. Nuclear Reactions in Stellar Interiors. H + H. 2 H + e + + nu. H + 2 H. 3 He + gamma. 3 He + 3 He. 4 He + H + H. Net effect: 4H 4 He. Question: why does this occur exclusively in the core of a star?. Demo.

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The HR Diagram

The HR Diagram. Astronomy 315 Professor Lee Carkner Lecture 8. Flux and Luminosity. How bright a star looks (W/m 2 ) How bright the star is (W) We measure the flux, but we want to know the luminosity. Inverse Square Law. What determines how bright a star looks?

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Stellar Evolution Life After the Main Sequence

Stellar Evolution Life After the Main Sequence. Stellar Evolution - Life After the Main Sequence Why Do Stars Evolve?. The Changing of Chemical Composition As a star uses fuel, it transforms light elements into heavy elements.

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Astronomy Division C

Science Olympiad. Astronomy Division C. Guidelines. Description: Students will demonstrate an understanding of the basic concepts of mathematics and physics relating to stellar evolution and Type II Supernova. A team of up to: 2 Approximate Time: 50 minutes. Guidelines.

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Earth Science 25.1 : Properties Stars

Earth Science 25.1 : Properties Stars. Properties of Stars. Earth Science 25.1 : Properties of Stars. The star P roxima Centauri is about 100 million times farther away from Earth than the moon. Yet, besides the sun, it is the closest star to Earth.

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Hertzsprung-Russell Diagram

There are thousands of stars that we can see with the naked eye. Stars can be classified into different categories . Hertzsprung-Russell Diagram . Hertzsprung-Russell Diagram . Different stars have different masses.

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UNIT NINE: Matter and Motion in the Universe

UNIT NINE: Matter and Motion in the Universe. Chapter 26 The Solar System Chapter 27 Stars Chapter 28 Exploring the Universe. Chapter Twenty-Seven: Stars. 27.1 The Sun 27.2 Stars 27.3 The Life Cycle of Stars. Chapter 27.2 Learning Goals. Compare the Sun to other stars.

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Announcements

Announcements. Vega. Comet SWAN!. West. Classifying the Stars. 27 October 2006. Today :. Stellar spectra: temperatures and compositions Are hotter stars brighter? (H-R diagrams) Determining sizes of stars Classifying stars, looking for patterns. Stellar Spectra. Pleiades Spectra.

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Binary stars and clusters

Binary stars and clusters. Chapter 11. Review. Properties of stars apparent brightness (apparent magnitude) measure energy/area/second luminosity (absolute magnitude) calculate distance, use inverse-square law distance to the star parallax temperature

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Star Clusters

Star Clusters. The Secret of the Stars http://www.youtube.com/watch?v=BuxFXHircaI Star clusters http ://www.spacetelescope.org/videos/heic1221a / Nebula and cluster in Milky way http://www.spacetelescope.org/videos/heic0715a /. 19.5 Shock Waves and Star Formation.

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Characteristics of Stars Chapter 3 Section 4 ISN p. 33

Characteristics of Stars Chapter 3 Section 4 ISN p. 33. What are stars?. The objects that heat and light the planets in a system A star is a ball of plasma and gas held together by its own gravity; they are much larger and hotter than planets due to nuclear fusion

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Properties of Stars

Properties of Stars. Chapter 30. Analyzing Starlight. Star- a large celestial body that is composed of gas and that emits light Nuclear fusion is the combination of light atomic nuclei to form heavier atomic nuclei Astronomers learn about stars by analyzing the light that the stars emit

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