'Red giant' diaporamas de présentation

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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Constellations & Stars

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HNRS 353 Chapter 11

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Stellar Evolution Review

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CHAPTER

CHAPTER. 4. Net Present Value. Chapter Outline. 4.1 The One-Period Case 4.2 The Multiperiod Case 4.3 Compounding Periods 4.4 Simplifications 4.5 What Is a Firm Worth? 4.6 Summary and Conclusions. 4.1 The One-Period Case: Future Value.

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Globular Clusters: HST Breathes New Life into Old Fossils

1. Globular Clusters: HST Breathes New Life into Old Fossils. Hubble Science Briefing Jay Anderson STScI June 3, 2010. 2. Outline. Globular Clusters Omega Cen Early release images Colors Simulations Stellar Populations The cutting edge with HST. 3. Globular Clusters.

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Stellar Evolution

Stellar Evolution. The Formation, Life and Death of the Stars. Star Birth I. Protostar Evolutionary Paths.

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Origin of the Solar System

Origin of the Solar System. Spiral Galaxy. Star Birth, Orion Nebula. Beta Pictoris. Solar Nebula. Formation of the Universe. Origin of the Solar System. Historically there have been two competing classes of hypotheses for origin of the solar system. 1. Dualistic or Encounter Hypothesis

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Origin of the Solar System

Origin of the Solar System. Spiral Galaxy. Star Birth, Orion Nebula. Beta Pictoris. Solar Nebula. Formation of the Universe. Origin of the Solar System. Historically there have been two competing classes of hypotheses for origin of the solar system. 1. Dualistic or Encounter Hypothesis

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Origin of the Solar System

Origin of the Solar System. Spiral Galaxy. Star Birth, Orion Nebula. Beta Pictoris. Solar Nebula. Formation of the Universe. Origin of the Solar System. Historically there have been two competing classes of hypotheses for origin of the solar system. 1. Dualistic or Encounter Hypothesis

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Stars and Nebulae

Stars and Nebulae. The study of the stars & nebulae provides information about the origin and history of the Earth and the solar system. Astronomers discover how stars like our Sun are born, grow old and die. Review. Pulsars are ...like neutron stars because....

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Nuclear Reactions

Nuclear Reactions. Nuclear Reactions. Binding Energies The mass law below represents the masses of thousands of nuclei with a few parameters B=(Z(m p +m e )+(A-Z)m n - M(A,Z))c 2 Mass Excess ?M = 9.31.478MeV (M(A,Z)-A) ; M in AMU

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Stellar Evolution

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Element Building in Large Stars

Element Building in Large Stars. Life Cycle of Stars - Part 2. Elements 2002 Workshop. Re: Principles of Stellar Evolution. The bigger it is, the hotter and the faster a star burns its life away. Energy released from nuclear fusion counter-acts inward force of gravity.

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LIFE AND DEATH OF STARS

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The Life Cycle of a Star

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Stellar Evolution

0. Stellar Evolution. 0. Evolution on the Main Sequence. Development of an isothermal core:. dT/dr = (3/4ac) ( k r/T 3 ) (L r /4 p r 2 ). MS evolution. Zero-Age Main Sequence (ZAMS). L r = 0 => T = const. 0. Interior of a 1 M 0 Star. X H (4.3 x 10 9 yr). X H (9.2 x 10 9 yr).

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Stars

Stars . How Stars are Classified. How bright a star looks depends on two factors: its magnitude, or brightness, and its distance from Earth. Two important terms to remember are: apparent and absolute magnitude.

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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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