Stars Evening Classes Week Three The Sun and Stars Presented by Oisín Creaner.

Slides:



Advertisements
Similar presentations
Life Cycle of Stars 1st Step: Stars form from nebulas
Advertisements

Chapter 16: Evolution of Low-Mass Stars
Review for Quiz 2. Outline of Part 2 Properties of Stars  Distances, luminosities, spectral types, temperatures, sizes  Binary stars, methods of estimating.
Objectives Determine the effect of mass on a star’s evolution.
Supernova. Explosions Stars may explode cataclysmically. –Large energy release (10 3 – 10 6 L  ) –Short time period (few days) These explosions used.
Energy Production in the Sun Physics 113 Goderya Chapter(s): 8 Learning Outcomes:
The Evolution of Stars - stars evolve in stages over billions of years 1.Nebula -interstellar clouds of gas and dust undergo gravitational collapse and.
What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion.
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.
Chapter 26 Part 1 of Section 2: Evolution of Stars
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 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,
Stars Star field taken with Hubble Space Telescope.
Objectives Determine the effect of mass on a star’s evolution.
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.
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.
Off the Main Sequence - The Evolution of a Sun-like Star Stages
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.
 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 
Stellar Structure Temperature, density and pressure decreasing Energy generation via nuclear fusion Energy transport via radiation Energy transport via.
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.
Intro screen.
$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.
Stars By: Mary Aragon Theory of Relativity. What are stars?  Enormous balls of gas  Made mostly of hydrogen and helium  Constant nuclear process (fusion)
Life Cycle of Stars Nebula hundreds of light years in size contract under gravity
A Note Taking Experience.
Life Cycle of Stars Birth Place of Stars:
Life Cycle of a Star A journey through it’s birth ‘til it’s death. By Anna, Damon, Shannon, Jon, and Patricia.
STARS.
Chapters 14 and 15 Stellar Evolution and Stellar Remnants.
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.
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.
The Life Cycle of Stars.
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.
Off the Main Sequence - The Evolution of a Sun-like Star Stages
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 CYCLE OF A STAR Objective: I will compare and contrast the life cycle of stars based on their mass.
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;
Stellar Evolution (Star Life-Cycle). Basic Structure Mass governs a star’s temperature, luminosity, and diameter. In fact, astronomers have discovered.
DAY 16 September 17, Agenda 1 st RP ‘Stuff’ back Grade Sheets Complete Star Notes Star Concept Map.
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.
Astronomy The Study of Planets, Stars, Galaxies, and More.
Stellar Evolution. Structure Mass governs a star’s temperature, luminosity, and diameter Hydrostatic Equilibrium – the balance between gravity squeezing.
Define Fusion Fusion is the combining of lighter atomic nuclei to make heavier atomic nuclei and energy. In the Sun, hydrogen is fused together to make.
Life Cycle of Stars 1st Step: Stars form from nebulas
Astronomy: Stars & Light
Option D2: Life Cycle of Stars
Chapter 30 Section 2 Handout
Section 3: Stellar Evolution
Life Cycle of Stars 1st Step: Stars form from nebulas
Nicholas Kellogg & Annessa strickland
Life Cycle of Stars 1st Step: Stars form from nebulas
(for low mass stars– like the Sun)
Life Cycle of Stars.
Life Cycle of Stars 1st Step: Stars form from nebulas
With thanks to Stellar Life Cycle With thanks to
Stellar Evolution It all depends On Mass.
Stars form from nebulas Regions of concentrated dust and gas
Birth out of the interstellar medium Contraction to a normal
Life Cycle of a Star.
From protostars to supernovas
The Sun.
Life Cycle of Stars 1st Step: Stars form from nebulas
Life Cycle of Stars 1st Step: Stars form from nebulas
Stellar Evolution Part 2 The fate of the Sun.
Chapter 17 The Sun.
The Sun and Other Stars 14-2.
The Sun.
Life Cycle of Stars 1st Step: Stars form from nebulas
Presentation transcript:

Stars Evening Classes Week Three The Sun and Stars Presented by Oisín Creaner

Corona Convective Zone Radiative Zone Photosphere Core Interior of the Sun

The Sun

Sunspots

The Sun

Causes of sunspots

Stellar Classes

Emission & Absorption Spectra

Binary Stars - the Doppler Effect!

Doppler Effect

Spectral Class of some well known stars

MASS-LUMINOSITY RELATIONSHIP L = M 35 01 35 = 01 x 01 x 01 x 01 = 1/3,000 th 2 35 = 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

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

Supernovae

The Sun in 5 billion years

Planetary Nebulae

White Dwarfs

Thank You Useful websites

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2024 SlidePlayer.com Inc. All rights reserved.