Topic 7.3 Continued Fission and Fusion

Slides:



Advertisements
Similar presentations
20th Century Discoveries
Advertisements

A nucleus can be specified By an atomic number and a Mass number.
Nuclear Fission & Fusion
A nucleus is more than just mass
Nuclear Fission & Fusion. History: Hahn & Strassman (1939) Bombarded Uranium-235 samples with neutrons expecting the Uranium-235 to capture neutrons Instead,
Fission reactor---mousetrap reactor video. Notes 43 - Topic 6 - Atomic and Nuclear Physics
Section 10–4: Fission and Fusion
Nuclear Chemistry L. Scheffler. The Nucleus The nucleus is comprised of the two nucleons: protons and neutrons. The number of protons is the atomic number.
Binding Energy Per Nucleon The binding energy per nucleon of a nucleus is the binding energy divided by the total number of nucleons in the nucleus Binding.
Topic : Nuclear Physics
Nuclear Fusion D-T Fusion Reactions. Nuclear fusion Nuclear fusion occurs when two light nuclei merge to form a heavier nucleus. The binding energy curve.
Nuclear Chemistry.
Atomic Stability. Isotopes Isotopes are atoms of an element that have different numbers of neutrons in their nucleus. Cu Copper – 63 OR Copper.
Fission Physics 12 Adv. Comprehension Check 1. Two deuterium nuclei fuse to form a tritium nuclei and a proton. How much energy is liberated? 2. A deuterium.
Atoms and Isotopes the light bulb is a reminder
Fission Lise Meitner- Austrian physicist during time of WWII. Discovered that bombardment of uranium with neutrons can split the nucleus into two pieces.
Nuclear Fusion By: Yours Truly, Christie Osadchy, and The Fool Who Ripped His Pants.
Fusion in the Stars Nunez & Panogalinog. Nuclear Fusion in stars is one of the most important reasons which make life on Earth possible! ○ HOW IS THAT.
½ - life The decay of a single nuclei is totally random However, with large numbers of atoms a pattern does occur.
NUCLEAR FUSION.
In your own words try to explain a radio active decay series
NUCLEAR CHEMISTRY. Atomic Structure Recall: Atoms – consist of a positively charged nucleus, which has protons and neutrons. IsotopeSymbol# protons# neutronsAtomic.
Nuclear Fission & Fusion. History: Hahn & Strassman (1939) Bombarded Uranium-235 samples with neutrons expecting the Uranium-235 to capture neutrons Instead,
Nuclear Fission and Fusion Chapter 10.2 Notes. Nuclear Forces Protons and neutrons are tightly packed inside the nucleus Remember that unstable nuclei.
Nuclear Chemistry. Radioactivity  Radioisotopes – isotopes that are unstable, who’s nucleus undergoes changes to gain stability  Radiation – the penetration.
CHAPTER 30 Nuclear Physics (Binding Energy, Nuclear Reaction)
Nuclear Stability You should be aware that: A nucleus can be naturally unstable Instability can be induced into a nucleus – for example if we bombard.
Dr. Bill Pezzaglia Nuclear Physics Updated: 2011Feb07 AstroPhysics Notes 1 Rough draft.
Dr. Bill Pezzaglia Nuclear Physics
Unit 7 Review Quiz #2 Solutions.
Atomic Energy 3U Physics.
Chapter 29: Nuclear Physics
Nuclear Physics.
The Atomic Nucleus & Radioactive Decay
½ - life The decay of a single nuclei is totally random
E = mc2 If you can’t explain it simply, you haven’t learned it well enough. Einstein.
Nuclear Chemistry 7.5.
Nuclear Fusion.
What is so dangerous about nuclear energy?
Nuclear Reactions.
Energy Unit Radioactivity.
Nuclear Energy Atoms and Isotopes.
Nuclear Stability Nuclear Changes
Nuclear Reactions November SCH 4U1 Mr. Dvorsky.
Notes 11.3: Radioactive Decay & Half-lives
Aim: What is Nuclear Chemistry
Nucleons Protons: +1 each, determines identity of element, mass of 1 amu, determined using atomic number, nuclear charge Neutrons: no charge, determines.
Nuclear Reactions PHY 3101 D. Acosta.
14.4 Chemical vs. Nuclear Reactions
Mass and Energy.
Multiple choice answers with explanation.
Chapter 10 Radioactivity and Nuclear reactions
Topic 7.3 Continued, 8.4 – Nuclear Power
Nuclear Energy Atoms and Isotopes.
Nuclear Chemistry.
The Nucleus Objectives:
AKA Radioactive DECAY or NUCLEAR DECAY
Nuclear Reactions.
Harnessing the Power of the Sun
AKA Radioactive DECAY or NUCLEAR DECAY
Dr. Bill Pezzaglia Nuclear Physics
Harnessing the Power of the Sun
Unit 7 Review Quiz #2 Solutions.
Chapter 14.4 Learning Goals
Nuclear Chemistry Chapter 21.
Nuclear Chemistry.
Can you fully describe the working of a nuclear reactor?
Nuclear Fission Elliott.
Nuclear Chemistry The energy of life.
Nuclear Chemistry.
Presentation transcript:

Topic 7.3 Continued Fission and Fusion

Nuclear Reactions Nuclear reactions produce very much more energy per particle than do chemical reactions. For example, the oxidization of one carbon atom produces about 4 eV of energy whereas the decay of a uranium atom produces about 4 MeV. However, natural radioactive isotopes do not occur in sufficient quantity to be a practical source of energy. It was not until the discovery of nuclear fission that the possibility of nuclear reactions as a cheap and abundant source of energy became possible.

Fission In 1934 Fermi discovered that when uranium was bombarded with neutrons, radioactive products were produced. Then in 1939 Hahn and Strassman showed that one of the radioactive products was barium (Z = 56). Enrico Fermi’s ID Badge Photo from Los Alamos

Fission It is now understood that a nucleus of uranium may capture a neutron to form an unstable isotope. Either of the following reactions may occur: where X and Y are two fission elements and x is the number of neutrons produced. Which reaction takes place is dependant on the energy of the bombarding neutron.

Fission as a Sustainable Energy Source The extra neutrons produced is the key to using fission as a sustainable energy source. Why? However, both the strontium isotope and xenon isotope produced are radioactive. Strontium-90 has a half-life of about 30 years and therein lies the main problem (as well as the large amounts of g-radiation also produced) with nuclear fission as a sustainable energy source – the fact that the fission nuclei are radioactive often with relatively long half-lives.

Little Boy The isotope uranium-235 also undergoes fission and much more readily than uranium-238. A typical fission reaction might be

Fusion Energy can also be obtained from nuclear reactions by arranging for two nuclei to “fuse” together as we alluded to when we discussed nuclear binding energy above. To produce nuclear fusion very high temperatures and pressures are needed so that nuclei can overcome the coulomb repulsion force between them and thereby come under the influence of the strong nuclear force. A typical nuclear reaction might be The energy released in this reaction is about 18 MeV.

Fusion The energy released appears in the form of kinetic energy of the helium nucleus and neutron. The advantage that fusion has compared to fission as a source of sustainable energy is that no radioactive elements are produced. This disadvantage is obtaining and maintaining the high temperature and pressure needed to initiate fusion.

Fission, Fusion, and the Binding Energy Curve The graph of binding energy per nucleon versus nucleon number shows that the nuclides with a nucleon number of about 60 are the most stable. This helps us to understand why the high nucleon number nuclides may undergo fission and the low nucleon number nuclides may under go fusion- they are trying to “reach” the nuclide that is most stable. Hence the sum of the total binding energies of the fission nuclei is greater than the total binding energy of the uranium-238 nucleus. Effectively the system has become more stable by losing energy. Similarly for the fusion reactions the total binding energy of the helium nucleus is greater than the sum of binding energies of the tritium and deuterium nuclei. So, again as for fission, the system has effectively become more stable by losing energy.

Fission, Fusion, and the Binding Energy Curve Hence the sum of the total binding energies of the fission nuclei is greater than the total binding energy of the uranium-238 nucleus. Effectively the system has become more stable by losing energy. Similarly for the fusion reactions the total binding energy of the helium nucleus is greater than the sum of binding energies of the tritium and deuterium nuclei. So, again as for fission, the system has effectively become more stable by losing energy.

Nuclear Fission and The Sun Our Sun is an enormous factory in which hydrogen is converted into helium. At some time in its early life, due to gravitational collapse of the hydrogen making up the Sun, the pressure and temperature of the interior became high enough to initiate fusion of the hydrogen. Once started, the fusion will continue until all the hydrogen is used up, probably in about 1010 years from now.

Nuclear Fission and the Sun One of the suggested fusion cycles that may take place in the Sun is For the complete cycle the first two reactions must occur twice and the final result is one helium nucleus, two positrons, two protons and two neutrinos. The protons are available for further fusion. In stars that are much more massive than our Sun, as they age fusion of elements with higher atomic numbers takes place until finally iron is reached and no further fusion can take place as seen from the binding energy graph.

Example:

Homework: Tsokos, Page 387 Questions 7 to14