Fusion Reactions in Stars

Slides:



Advertisements
Similar presentations
Life as a Low-mass Star Image: Eagle Nebula in 3 wavebands (Kitt Peak 0.9 m).
Advertisements

Stellar Evolution. The Mass-Luminosity Relation Our goals for learning: How does a star’s mass affect nuclear fusion?
Review for Quiz 2. Outline of Part 2 Properties of Stars  Distances, luminosities, spectral types, temperatures, sizes  Binary stars, methods of estimating.
Nucleosynthesis Elements are made in four distinct ways (plus another we didn’t go into)  Big Bang Nucleosynthesis  takes place when the universe is.
Where do elements come from?. Remember the Big Bang? The theory states that Universe today retains an imprint of its initial cosmic mixture of elements.
GEOL3045: Planetary Geology Lysa Chizmadia 11 Jan 2007 The Big Bang & Nucleosynthesis Lysa Chizmadia 11 Jan 2007 The Big Bang & Nucleosynthesis.
The origin of the (lighter) elements The Late Stages of Stellar Evolution Supernova of 1604 (Kepler’s)
Introduction to nuclear physics Hal. Nucleosynthesis Stable nuclei.
© G. Hill and A. Hunt 2008 Edexcel Chemistry for AS 1 Chemical quantities.
After the Sun's core hydrogen is depleted by nuclear fusion the core will consist primarily of 1) carbon. 2) deuterium. 3) helium. 4) oxygen.
Stellar Interiors Physical Astronomy Professor Lee Carkner Lecture 10.
Stars: Nuclear Furnaces. Elemental Composition of Universe.
History of the Earth Chapter 1: Formation of the Earth From the Big Bang to Early Planets.
Activity #32, pages (pages were done last Friday)
 Produced during the Big Bang  Hydrogen, Helium and lithium.
Life Track After Main Sequence
Stars start out as a Nebula –
Creation of the Elements Chapter 4 Section 4. Hydrogen was formed from energy after the Big.
Stellar Fuel, Nuclear Energy and Elements How do stars shine? E = mc 2 How did matter come into being? Big bang  stellar nucleosynthesis How did different.
How do you read the PERIODIC TABLE? What is the ATOMIC NUMBER? o The number of protons found in the nucleus of an atom Or o The number of electrons surrounding.
The Nuclear Fusion Reaction Inside Stars Investigative Science Lab book pages
Chemistry Connections to the Universe Kay Neill, Presenter.
Creation of the Chemical Elements By Dr. Harold Williams of Montgomery College Planetarium
ELEMENTS atomic number = Z = number of protons = p mass number = number of nucleons = p + n atomic mass = experimental measurement of the mass of the.
Stellar Structure Temperature, density and pressure decreasing Energy generation via nuclear fusion Energy transport via radiation Energy transport via.
Lecture 24: Life as a High-Mass Star. Review from Last Time: life for low-mass stars molecular cloud to proto-star main sequence star (core Hydrogen burning)
Chapter 17 Star Stuff.
Lesson 13 Nuclear Astrophysics. Elemental and Isotopic Abundances.
H205 Cosmic Origins  Our last class!  Origin of the Elements  Hand in EP7 APOD Tom Lehrer's "The Elements". A Flash animation by Mike Stanfill, Private.
The Reactions The Main Sequence – The P – P Chain 1 H + 1 H  2 H + proton + neutrino 2 H + 1 H  3 He + energy 3 He + 3 He  4 H + 1 H + 1 H + energy.
12.3 Life as a High-Mass Star Our Goals for Learning What are the life stages of a high mass star? How do high-mass stars make the elements necessary for.
Basic Physical Principles Lancelot L. Kao Updated: Jan 18, 2010.
Video Questions What elements were created during the big bang?
Two types of supernovae
Stellar Spectroscopy and Elemental Abundances Definitions Solar Abundances Relative Abundances Origin of Elements 1.
Chapters 14 and 15 Stellar Evolution and Stellar Remnants.
Question 1: The CNO cycle, Review Quiz No. 13 :60 1.involves the fusion of Carbon, Nitrogen, and Oxygen into heavier elements. 2.involves the fission of.
The Reactions The Main Sequence – The P – P Chain 1 H + 1 H  2 H + proton + neutrino 2 H + 1 H  3 He + energy 3 He + 3 He  4 H + 1 H + 1 H + energy.
Welcome– 10/17 Collect Lab Reports Big Bang Theory and Life Cycle of the Star Notes Nuclear Chemistry Notes HW: NONE!
Selected Topics in Astrophysics. Solar Model (statstar) Density Mass Luminosity Temperature Nuclear Reaction Rate Pressure.
Review Quiz No. 16 :60 1.A0 2.B2 3.F5 4.K2 5.G2 Question 1: Stars of which of the following spectral types have the shortest main- sequence life time?
After the Big Bang. ENERGY & MASS The infant Universe was searingly HOT! It was full of energy of intense radiation. Albert Einstein’s equation E=mc2.
Alpha Fusion in Stars An explanation of how elements on the periodic table, from He to Fe, are produced in stars such as Red Giants and Super Giants. AUTHORS:
Earth in Space Benchmarks
Define - Physical change? Give an example of a Physical change.
Announcements Second hour exam is this Friday, October 8
Measuring Stellar Reaction Rates with Bubble Chamber
Stellar Evolution Pressure vs. Gravity.
Hydrogen Burning (Proton-proton chain)
Elemental Composition of the Universe
2.1 / BIG BANG THEORY REVIEW GAME.
Supernova Neutron Star Planetary Nebula.
Chapter 12 Supernova Remnant
Where do chemical elements come from?
From Birth to Death (Dust to Dust)
ISOTOPES Isotopes are atoms of the same element that have a different number of neutrons. They differ in mass, but the atom’s chemical behavior are.
Nucleosynthesis and the origin of the chemical elements
Creation of the Chemical Elements
BLACK HOLES By: Ruby Hayes-Baum.
Supernova.
Matter.
Origin of Elements.
Name the 3 subatomic particles?
p p → Fusion Reactions in Stars Hydrogen “Burning “ at 107 K
The Chemistry of the Solar System
Nucleosynthesis and the origin of the chemical elements
CHAPTER 3 The Raw Material 강재중.
STELLAR EVOLUTION. STELLAR EVOLUTION What is a star? A star is a huge ball of hot gas, held together by its own gravity. Most of the gas is hydrogen.
Atomic Structure.
Chapter 3, Part2 Nuclear Chemistry CHEM 396 by Dr
Presentation transcript:

Fusion Reactions in Stars A Hydrogen burning at 107 K p-p chain reaction Harry Kroto 2004

Fusion Reactions in Stars A Hydrogen burning at 107 K p-p chain reaction Harry Kroto 2004

Fusion Reactions in Stars A Hydrogen burning at 107 K p-p chain reaction Harry Kroto 2004

Helium Burning at 108K Harry Kroto 2004

Harry Kroto 2004

Carbon Burning at 5x108 K Harry Kroto 2004

Silicon burning at 2x109 K Harry Kroto 2004

Harry Kroto 2004

The Origin of the Elements The Big Bang H D 3He 4He 7Li (No stable mass 5 and 8) Harry Kroto 2004

The Origin of the Elements The Big Bang H D 3He 4He 7Li (No stable mass 5 and 8) Stellar interiors C to Fe (and some He) Harry Kroto 2004

The Origin of the Elements The Big Bang H D 3He 4He 7Li (No stable mass 5 and 8) Stellar interiors C to Fe (and some He) Supernovae Elements with mass > Fe Harry Kroto 2004

CN cycle 107 K Harry Kroto 2004

Oxygen burning at 109K Harry Kroto 2004

The Synthesis of the Elements Summary The Synthesis of the Elements Harry Kroto 2004

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

© 2025 SlidePlayer.com. Inc. All rights reserved.