Student s Question of the Day. What is Nuclear Fusion?

Similar documents
Student s Question of the Day

Section 2: Nuclear Fission and Fusion. Preview Key Ideas Bellringer Nuclear Forces Nuclear Fission Chain Reaction Nuclear Fusion

Atomic and Nuclear Physics. Topic 7.3 Nuclear Reactions

DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS

Matter and Energy. Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law.

DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS

Nuclear Fusion 1 of 24 Boardworks Ltd 2011

LECTURE 25 NUCLEAR STRUCTURE AND STABILITY. Instructor: Kazumi Tolich

Fission & Fusion Movie

An introduction to Nuclear Physics


Fundamental Forces of the Universe

Stellar energy generation on the main sequence

Chapter 10 Section 4 Notes

10.4 Fission and Fusion

Lecture 14, 8/9/2017. Nuclear Reactions and the Transmutation of Elements Nuclear Fission; Nuclear Reactors Nuclear Fusion

Modeling the Interactions in a Nucleus

Forces and Nuclear Processes

Unit 1 Atomic Structure

FUSION NEUTRON DEUTERIUM HELIUM TRITIUM.

Unit 1 Atomic Structure

Lesson 1: The Sun. Reading Assignment. Summary of Fundamental Forces

[2] State in what form the energy is released in such a reaction.... [1]

turbine (a) (i) Which part of the power station provides thermal (heat) energy from a chain reaction?

The Twinkle in Mother Earth s Eye: Promising fusion power. What if you could have a miniature star powering your house, your computer, and your car?

Slide 1 / 57. Nuclear Physics & Nuclear Reactions Practice Problems

[1] (c) Some fruits, such as bananas, are naturally radioactive because they contain the unstable isotope of potassium-40 ( K.

Friday, 05/06/16 6) HW QUIZ MONDAY Learning Target (NEW)

THE NUCLEUS OF AN ATOM

Science 10: Radioactivity! Comparing Fission and Fusion Notes (Ch 11)

Nuclear fission and fusion are processes that involve extremely large amounts of energy.

Aim: What are the two types of Nuclear. Reactions? Do Now: 1. Get into your groups and compare your answers to your homework.

Structure of the Nuclear Atom

NUCLEI. Atomic mass unit

Recap I Lecture 41 Matthias Liepe, 2012

Nuclear Reactions. Fission Fusion

Jacob s Ladder Controlling Lightning

A is called the mass number gives, roughly, the mass of the nucleus or atom in atomic mass units = amu = u

Nuclear Physics and Nuclear Reactions

The Atomic Nucleus & Radioactive Decay. Major Constituents of an Atom 4/28/2016. Student Learning Outcomes. Analyze radioactive decay and its results

Alta Chemistry CHAPTER 25. Nuclear Chemistry: Radiation, Radioactivity & its Applications

AST 100 General Astronomy: Stars & Galaxies

Multiple Choice Questions

There are 82 protons in a lead nucleus. Why doesn t the lead nucleus burst apart?

Today. Homework Due. Stars. Properties (Recap) Nuclear Reactions. proton-proton chain. CNO cycle. Stellar Lifetimes

Term 3 Week 2 Nuclear Fusion & Nuclear Fission

General Physics (PHY 2140)

Holding the Nucleus Together

PHYS 420: Astrophysics & Cosmology

James Maxwell ( )

Fusion in stars and on Earth Tokamaks and the Hot CNO cycle

Lecture Outlines Chapter 32. Physics, 3 rd Edition James S. Walker

Nuclear Binding Energy

Nuclear Physics and Radioactivity

Atomic Quantum number summary. From last time. Na Optical spectrum. Another possibility: Stimulated emission. How do atomic transitions occur?

Today. Stars. Properties (Recap) Binaries. Stellar Lifetimes

Unit 6 Nuclear Radiation Parent Guide. What is radioactivity and why are things radioactive?

The Sun. the main show in the solar system. 99.8% of the mass % of the energy. Homework due next time - will count best 5 of 6

Lecture 31 Chapter 22, Sections 3-5 Nuclear Reactions. Nuclear Decay Kinetics Fission Reactions Fusion Reactions

Chemistry Review Unit 1 Study Guide

The Sun Our Nearest Star The Sun is an average star in mass, lifetime, and energy output. We will look at in detail before studying stars in general

β and γ decays, Radiation Therapies and Diagnostic, Fusion and Fission Final Exam Surveys New material Example of β-decay Beta decay Y + e # Y'+e +

Nuclear Chemistry. Mass Defect. E=mc 2. Radioactivity. Types of Radiation. Other Nuclear Particles. Nuclear Reactions vs. Normal Chemical Changes

UNIT 13: NUCLEAR CHEMISTRY

Fission and Fusion Book pg cgrahamphysics.com 2016

! Exam 1 in this classroom in 1 week (Oct 1 st )! 40 Multiple choice questions! Will cover material up to and including today.!

Nuclear Energy 6/04/08. Lecture 22 1

Nuclear Physics (chapters 14 & 15) strong societal themes and impact!

Nuclear Reactions A Z. Radioactivity, Spontaneous Decay: Nuclear Reaction, Induced Process: x + X Y + y + Q Q > 0. Exothermic Endothermic

Chemistry Unit 2 Quiz KEY

PHYS 202. Lecture 24 Professor Stephen Thornton April 27, 2005

Nuclear power plants can generate large amounts of electricity.

LIFE CYCLE OF A STAR

Nuclear Energy Learning Outcomes

Nuclear Energy Learning Outcomes. Nuclear Fission. Chain Reaction

Radioactivity is the spontaneous disintegration of nuclei. The first radioactive. elements discovered were the heavy atoms thorium and uranium.

Nuclear Energy. Nuclear Structure and Radioactivity

Organizing the Elements (pages )

AN OVERVIEW OF NUCLEAR ENERGY. Prof. Mushtaq Ahmad, MS, PhD, MIT, USA

Solar Fusion. After Steele Hill, SOHO

State the main interaction when an alpha particle is scattered by a gold nucleus

Erasmus Plus INS Ramon Berenguer IV LESSON PLAN

Nuclear Energy; Effects and Uses of Radiation

Basic Nuclear Theory. Lecture 1 The Atom and Nuclear Stability

Electromagnetic Waves

10/20/2009. Giants, Dwarfs, and the Main Sequences. My Office Hours: Tuesday 3:30 PM - 4:30 PM 206 Keen Building. The Sun and the Stars

Section 1: Atoms. Suggested Films. What Is An Atom? Discovery of the Atom

SAVE PAPER AND INK!!!

Lecture PowerPoints. Chapter 31 Physics: Principles with Applications, 7th edition Giancoli

WELCOME TO PERIOD 20: RADIANT ENERGY FROM THE SUN

Chapter 10 - Nuclear Physics

BIG BANG SUMMARY NOTES

Nuclear Chemistry Lecture Notes: I Radioactive Decay A. Type of decay: See table. B. Predicting Atomic Stability

LIFE CYCLE OF A STAR

Quantum Mechanics. Exam 3. Photon(or electron) interference? Photoelectric effect summary. Using Quantum Mechanics. Wavelengths of massive objects

Chem!stry. Notes on Atomic Structure Macroconcept: Models

Journal 14. What is so dangerous about nuclear energy?

Limb Darkening: The Inside of the Sun: What keeps the Sun shining? What keeps the Sun from collapsing? Gravity versus Pressure. Mechanical Structure

The Sun = Typical Star

Announcements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11

Transcription:

COMSATS Institute of Information Technology Department of Physics Defense Road, Lahore, Pakistan January-February, 2009 In this issue Student s Question of the Day New Research Not wonder, this is Physics News Bulletin Photo Gallery Vol.06-07 Patron: Dr. S. A. Hayat Chairman: Dr. A. S. Bhatti Editor in chief: Dr. A. Ashfaq Editors: Dr. Ejaz A Mughal / Dr. A Rashid / Ms. S. Aslam Student s Question of the Day What is Nuclear Fusion? Nuclear fusion involves the bringing together of atomic nuclei. The atom's nucleus consists of protons (p) with a single positive charge and neutrons (n) of similar mass and no charge. The strong nuclear force holds these "nucleons" together against the repulsive effect of the proton's charge. As many negatively charged electrons as protons swarm around the nucleus to balance the proton charge and the mass of the atom lies almost totally in the nucleus. The sum of the individual masses of the nucleons is greater than the mass of the whole nucleus. This is because the strong nuclear force holds the nucleons together - the combined nucleus is a lower energy state than the nucleons separately. The difference, the binding energy ( E= mc 2 ), varies from one element to another. Because of the possible ways that nucleons can pack together, Fig 1: Comparison of Energy released in Fission and Fusion. when two light atomic nuclei are brought together to make a heavier one, the binding energy of the combined nucleus can be more than the sum of the binding energies of the component nuclei (i.e. it is in an even lower energy state). This energy difference is released in the "fusion" process. A similar situation occurs when heavy nuclei split. Again the binding energies of the pieces can be more than that of the whole (i.e. they are in a lower energy state), and the excess energy is released in

the "fission" process. These alternatives are shown in the Figure 1. In the Sun and stars a chain of fusion reactions (see Table 1) occur which converts hydrogen to helium. There are two chains, both having the same effective result, and which one dominates depends on the size of the star. For our Sun the proton cycle dominates. Table1: Proton cycle and Carbon-Nitrogen-Oxygen Cycle. Fig 2: "Reactivity" - the product of the probability of reaction and the energy delivered per reaction. The overall reaction rate is extremely low, but it nevertheless drives the universe due to star sizes and huge masses. The particles are held together by gravity long enough for sufficient reactions to occur. For instance, in the core of the Sun the temperature is 10-15 million C. Along with the extreme pressure (a quarter of a trillion atmospheres) and density (eight times that of gold), this allows matter to be converted into large amounts of energy. To make fusion on a smaller scale on earth, more probable reactions have to be used. A figure of merit for a reaction is the "reactivity" - the product of the probability of reaction and the energy delivered per reaction as shown in figure 2. Fig. 3: The fusion reaction between two "isotopes" of hydrogen, deuterium (D) and tritium (T). In Figure 3 (for a given confinement capability) shows, the fusion reaction between two "isotopes" of hydrogen, deuterium (D) and tritium (T), has maximum reactivity at around 100 million C (isotopes have the same number of protons, but a different number of neutrons).the next most reactive is D+D, about 40 times smaller, and

D+ 3 He, an isotope of helium, about 85 times smaller. The D+D reactivity value includes "side reactions" between D and the D+D reaction products, namely T and 3 He. For comparison, the reactivity of stellar reactions is 3 x 10-25 smaller than that for D+T. This large difference allows fusion power to be a possibility on human scales, but the removal of the large mass which allows gravitational confinement to work so well in stars means that different confinement schemes have to be exploited, and these have different conditions for their success. Dr. Muhammad Asif (Assistant Professor, Physics, CIIT Lahore) New Research A search group in USA has recently designed absorbing left-handed materials having nearly unity absorbance. The design uses the exotic behavior of left- handed elements that individually absorb completely the electric and magnetic field component of the electromagnetic wave impinging on it. Physical Review Letter 100,207402 (2008) Not wonder, this is Physics The energy of empty space is called "zero-point" energy. Its density is same throughout the universe. As the universe expands and space grows larger, the amount of "zero-point" energy also grows ever larger. Hence this "zero-point" energy is being created by the universe constantly thus violating the conservation of energy. So zero-point" energy is contributing to the continuing expansion of the universe News Bulletin 1. Dr. Samar Mubarak Mand, renowned scientist and member Pakistan Planning Commission visited CIIT, Lahore campus on January 10, 2009. During the visit to Physics Department, Dr. Samar Mubarak Mand appreciated the role of physicists in the scientific advancement of Pakistan, and emphasized on the conceptual learning and active involvement of students in the research activities. 2. Dr. Shabana Nisar of Syracuse University USA delivered a talk titled, The Subatomic Cosmos and the Tools of Discovery on January 19, 2009, at 12.10 P.M, in the seminar room of Block A. 3. Dr. Arshad Saleem Bhatti Chairman Department of Physics CIIT, Islamabad delivered a talk titled, Bio-Sensors: New Avenues for Physicist and Engineers on February 12, 2009, at 2.00 P.M, in the seminar room of Block A 4. Prof. Dr. Mirko Cvjeticanin, Director Middle East PHYWE had a wonderful interactive session with the faculty and students of CIIT, Lahore on February 24, 2009, at 11.00 A.M, in the seminar room of Block A. The main focus

of the talk was that why we need natural sciences more than ever? Dr. Mirko pointed out that we need the knowledge of Biology, Chemistry and Physics to support all the advancements in the area of science and technology such as Oil and gas, Energy, Soft ware, Entertainment, Pharmaceutical, Textile, Telecom, Agriculture, Material Coating, Chemical Industry, Metal Forging etc 5. A research paper by Dr. Muhammad Asif titled, Relationship between current density and mass density for ohmic tokamak plasmas has been published in International Journal of Modern Physics B, 22 (2008) 5329. Photo Gallery Some of glimpses of the great moments of the visit of Dr. Samar Mubarak Mand to the Physics Department and Seminars held in the Physics Department are posted below.

JOIN COMSATS PHYSICS FORUM Objectives of the Forum Arrangement of Seminars / workshops Arrangement of educational trips Organization of Co-Curricular activities e.g. Quiz competition, Research and general paper reading contest etc FREE MEMBERSHIP OPEN FOR ALL Contact: Secretary COMSATS Physics Forum Dr. Abdul Rashid COMSATS Institute of Information Technology Defence Road, off- Raiwind Road Lahore. Phone: 111-001-007 / ext.235, 295 Fax: 042-9203100 Cell Phone: 0332-4331077 E-mail: drabdulrashid@ciitlahore.edu.pk URL: www.ciitlahore.edu.pk

COMSATS PHYSICS FORUM MEMBERSHIP FORM Name ------------------------------------------ Institute----------------------------------- E-mail ----------------------------------- Field of Research/interest---------- No. of International Publications-------- Qualification------------------ Designation-------------------- Cell No.--------------------------- Research/Teaching Experience------ No. of Local Publications---------- Signature of the applicant Nominated/Recommended by Head of the Institute: Signature:-------------- Name:----------------------- Institute:-------------------- For Office Use: Membership is recommended: Yes No Membership No.------------------ Dated: -------------------- Secretary COMSATS Institute of Information Technology Department of Physics, M. A. Jinnah Campus Defence Road, off Raiwind Road, Lahore 54000, Pakistan Tel: 042-5321094 Fax: 042-9203100 URL: www.ciitlahore.edu.pk