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Stars Evening Classes Week Three The Sun and Stars Presented by Oisín Creaner
Corona Convective Zone Radiative Zone Photosphere Core Interior of the Sun
Causes of sunspots
Emission & Absorption Spectra
Binary Stars - the Doppler Effect!
Spectral Class of some well known stars
MASS-LUMINOSITY RELATIONSHIP L = M 35 01 35 = 01 x 01 x 01 x 01 = 1/3,000 th 2 35 = 2 x 2 x 2 x 2 = 11 5 = 100 x 100 x 100 x 100 = 10 million.
Stars Evening Classes Week Three Presented by Oisín Creaner
Hydrostatic Equilibrium The collapsing nebula’s core is squeezed by gravity
Hydrostatic Equilibrium It reaches 10 million degrees.
P P P Extent of electro- magnetic force (repulsive) Extent of strong nuclear force (attractive)
Hydrostatic Equilibrium Balance between gravitation & thermal expansion
Core Helium Enrichment
Helium Core Hydrogen fusing shell
Helium Core Hydrogen fusing shell
Helium Core Hydrogen Envelope
A Star’s Life - Death After the main sequence
The Sun in 5 billion years
Thank You Useful websites
Stars Star field taken with Hubble Space Telescope.
Chapters 14 and 15 Stellar Evolution and Stellar Remnants.
Stellar Evolution. Structure Mass governs a star’s temperature, luminosity, and diameter Hydrostatic Equilibrium – the balance between gravity squeezing.
The Life Cycle of Stars. Stars are huge masses of gas with a massive gravitational pull that keeps the planets orbiting around them. They also give out.
Off the Main Sequence - The Evolution of a Sun-like Star Stages
Energy Production in the Sun Physics 113 Goderya Chapter(s): 8 Learning Outcomes:
Birth Place of Stars: Dark and cold inter-stellar clouds These clouds are made of more hydrogen than helium. These clouds have very small amount of heavier.
DAY 16 September 17, Agenda 1 st RP ‘Stuff’ back Grade Sheets Complete Star Notes Star Concept Map.
The Lives of Stars. Topics that will be on the test!! Apparent and Absolute Magnitude HR Diagram Stellar Formation and Lifetime Binary Stars Stellar Evolution.
Life Cycle of Stars. Star Birth Develops from nebula –Nebula is a collection of dust and gas Gravity overcomes pressure Gravitational contraction.
LIFE OF A STAR BY: STACIA DEUTSCH AND RHODY COHON.
Review for Quiz 2. Outline of Part 2 Properties of Stars Distances, luminosities, spectral types, temperatures, sizes Binary stars, methods of estimating.
THE LIFE CYCLE OF A STAR Objective: I will compare and contrast the life cycle of stars based on their mass.
The Evolution of Stars - stars evolve in stages over billions of years 1.Nebula -interstellar clouds of gas and dust undergo gravitational collapse and.
Stars By: Mary Aragon Theory of Relativity. What are stars? Enormous balls of gas Made mostly of hydrogen and helium Constant nuclear process (fusion)
STARS & their life cycles Like us, stars are born, grow older, become middle aged and eventually die!!! Unlike us, stars take billions of years to complete.
$1 Million $500,000 $250,000 $125,000 $64,000 $32,000 $16,000 $8,000 $4,000 $2,000 $1,000 $500 $300 $200 $100 Welcome.
Stellar Evolution – Life of a Star Stellar evolution is the process in which the forces of pressure (gravity) alter the star. Stellar evolution is inevitable;
Astronomy The Study of Planets, Stars, Galaxies, and More.
Star Structure Diagram (Draw this) Star Structure The sun, like all stars, is made up of hydrogen and helium gases, and a handful of other elements depending.
Stellar Evolution (Star Life-Cycle). Basic Structure Mass governs a star’s temperature, luminosity, and diameter. In fact, astronomers have discovered.
Stars Earth Science – Mr. Foster. Why do stars exist? Stars exist because of gravity Two opposing forces in a star are – Gravity – contracts – Thermal.
The life and death of stars. How do stars work and evolve? Why do stars shine? –Nuclear reactions Fusion and fission reactions How nuclear reactions can.
THE LIFE CYCLES OF STARS. In a group, create a theory that explains: (a)The origin of stars Where do they come from? (b)The death of stars Why do stars.
STARS. Life Cycle of A Star 1. Stars begin their lives as clouds of dust and gas called a stellar nebula.
Astronomy Picture of the Day. The Sun Core temperature - 15 million K Surface temperature K 99.9% of all of the matter in the solar system Entirely.
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.
Objectives Determine the effect of mass on a star’s evolution. Identify the features of massive and regular star life cycles. Explain how the universe.
Supernova. Explosions Stars may explode cataclysmically. –Large energy release (10 3 – 10 6 L ) –Short time period (few days) These explosions used.
The Layers of a Star The corona is the wide, outermost layer of a Sun’s atmosphere – (AL) The chromosphere is the orange-red layer of the Sun’s atmosphere,
Life Cycle of Stars Nebula hundreds of light years in size contract under gravity
The Life Cycle of Stars A Note Taking Experience..
What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion.
Stellar Structure Temperature, density and pressure decreasing Energy generation via nuclear fusion Energy transport via radiation Energy transport via.
A star is a ball of hydrogen, helium and enough mass that can bear nuclear fusion at its core Stars are most often seen at night in a clear sky
Life Cycle of a Star A journey through it’s birth ‘til it’s death. By Anna, Damon, Shannon, Jon, and Patricia.
I Life Cycle of the Sun: A. Stars are born in nebulas. B. Nebula- A rapidly condensing cloud of gas and dust. C. Star “Pre-life Steps” 1. Gases rapidly.
Classifica tion HR diagram Star clusters TermsLife cycle Black holes Life Cycles 2 $ 200 $ 200$200 $ 200 $ 200 $400 $ 400$400 $ 400$ $600 $
Lives in the Balance Life as a Low Mass Star. Star mass categories: Low-mass stars: born with less than about 2 M Sun Intermediate-mass stars: born with.
Chapter 26 Part 1 of Section 2: Evolution of Stars.
1 Stellar Lifecycles The process by which stars are formed and use up their fuel. What exactly happens to a star as it uses up its fuel is strongly dependent.
Nebula to Protostar Giant molecular clouds within a nebula contract under the gravitational pressure, increasing its thermal energy. CO, NO, OH- Giant.
Star Formation. Introduction Star-Forming Regions The Formation of Stars Like the Sun Stars of Other Masses Observations of Brown Dwarfs Observations.
Chapter 16: Evolution of Low-Mass Stars. While on the Main Sequence stars of all mass burn hydrogen into helium.
The Sun Chapter Standard O 8.2.g. Students know the role of gravity in forming and maintaining the shapes of planets, stars and the solar system.
Stars Chapter 25. The Sun The Sun’s mass controls the motions of the planets Less dense than Earth High pressure and temperature causes gases to be plasma.
Life Cycle of a Star STAR NURSERY The star nursery is called the Nebula. Spaces acts as a nursery full of the gases and dust that stars need to.
Stellar Deaths Novae ans Super Novae 16. Hydrostatic Equilibrium Internal heat and pressure from fusion pushes outward Gravity pulling mass inward Two.
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