'Main sequence' presentation slideshows

Main Sequence Lifetimes

Main Sequence Lifetimes. Time on Main Sequence How much fuel it has (Core H) How fast it consumes the fuel (Luminosity). Main Sequence Lifetimes. Main Sequence Lifetimes. Our Sun M = 1 M ( ?) and L = 1 L ( ?) t MS -lifetime = 10 10 years = 10 billion years

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HNRS 353 Chapter 11

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Stars & Galaxies

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The Evolution and Explosion of Massive Stars

The Evolution and Explosion of Massive Stars. Cornell Physics Colloquium, February 25, 2002. see also Reviews of Modern Physics , S. E. Woosley, A. Heger, and T. A. Weaver, in press (2002) http://www.supersci.org. Supernovae:. Make brilliant fireworks.

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Spectrum Synthesis and Supernovae

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THE FAMILY OF STARS

THE FAMILY OF STARS. Corresponds to Ch 6 in book Astro by Seeds Prepared by: Julissa Garcia , Aramik Yousefian Hagop Hadjinian , Tatevik Grigoryan Activity director: Lilit Haroyan Faculty Advisor: Richard Rains. START. EXIT.

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Dimensions of Stars

Dimensions of Stars. Having determined that stars are at large distances, high temperatures and very luminous, the next question to ask is how large they are. An Example:. Dimensions of Stars. The star Betelgeuse ( a Orionis) has the following parameters: Distance 150 pc

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Evolution of Stars

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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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STARS

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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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A bit about me!

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Space Science Unit Quick overview:

Space Science Unit Quick overview: Galaxies Multiple Star Systems Constellations Spectroscope Lab Toilet Paper Solar System Lab Characteristics of Stars H-R Diagram Measuring Star distances (parallax) The Sun: Our special Star Activities of the Sun Introduction Activity

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Stars

Stars. Other Suns. Physical Properties. Luminosity Mass Diameter (radius) Must know distance to find out these properties!. Physical Properties. Surface temperature Chemical composition Analyze spectra to infer these properties; distance not required. Distances.

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Academic Writing

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1st Step: Stars form from nebulas Regions of concentrated dust and gas Gas and dust begin to collide, contract and heat

Life Cycle of Stars. 1st Step: Stars form from nebulas Regions of concentrated dust and gas Gas and dust begin to collide, contract and heat up All due to gravity. Life Cycle of Stars. 2nd Step: As nebula contracts, a small star is formed Called a protostar

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Habitability: Earth to Universe

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Evolution of the Solar System

Evolution of the Solar System. Matt Rogers AT350 9 September 2003. Overview. Evolution of a star Interstellar Nebula Formation of protostar and protostellar nebula Evolution of early sequences and dissipation of protostellar nebula. Overview (continued). Evolution of planets

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Stars

Stars. Distances To The Stars. Stars are separated by vast distances. Astronomers use units called light years to measure the distance of stars A light-year is the distance that light travels in a vacuum in a year Proxima Centauri, is the closest star to the sun.

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