Calculating the Lifetime of the Sun
|
|
|
- Clemence Edwards
- 7 years ago
- Views:
Transcription
1 Calculating the Lifetime of the Sun
2 What would you need to know in order to decide how much time you have before a car runs out of gas? How much gas you have in the tank. (gallons) How fast you are burning that fuel. (gallons/hour) Suppose you have a full tank of gas and for your car that is 12 gallons. You drive for one hour at a constant rate and after that hour you notice the gas gauge is ¾ full. This means that you are burning 3 gallons/hour. If you continue at this rate, what is the total possible travel time?
3 What is the total travel time? 1. 2 hours 2. 3 hours 3. 4 hours 4. 5 hours
4 To figure out the total time you need to divide the amount of fuel by the rate of consumption. Total time = (12 gallons)/(3 gallons/hour) Total time = 4 hours. Notice that the gallons cancel and when you invert and multiply the hours come up on top.
5 Finding the lifetime of the Sun is a very similar problem 4H He + energy (Nuclear reaction) So four hydrogen atoms are changed into Helium atoms and energy is released. Once the hydrogen is gone, so is the fuel supply. We need to know how much fuel is in the Sun and how fast it is being used up.
6 To know the amount of fuel in the Sun we need to know the Sun s mass. To know how fast the fuel is being used up we need to know the Sun s luminosity (watts). It is also important to know the composition of the Sun: 71% Hydrogen, 27% Helium and 2% the other 90 elements.
7 Luminosity We know that the luminosity (the energy leaving the Sun every second) has to be equal to the amount of energy being produced in the core of the Sun, every second. Otherwise the Sun would either expand or shrink. So how can we find the Luminosity of the Sun?
8 Imagine a detector in orbit around the Earth. This detector is 1 meter 2. The detector captures the EM radiation coming from the Sun and shows that there is 1357 watts hitting the detector. Is this the luminosity of the Sun? What would you have to do in order to determine the entire amount of energy leaving the Sun?
9 5 How can you determine the Sun s luminosity? Build enough detectors to completely surround the Sun and add up all the values. 2. Use the value for one detector and multiply it by the total area around the Sun 3. Assume that the one detector is pretty close to right. 0% 0% 0%
10 The Luminosity can be found by multiply the energy/second falling on the detector, by the total surface area of a sphere with a radius of the Earth s orbit. L = B(4πd 2 ) Where B is the apparent brightness in units of watts/meter 2 and d is the distance to the Sun. L = (1357 watts/m 2 )(4π)(1.5 x meters) 2 L = 3.8 x watts or (joules/second) Total World Wide energy consumption for the year of 2005 was 5 x Joules. That is onemillionth of the energy that leaves the Sun every second.
11 We know that the energy leaving the Sun every second is equal to the energy being produced in the core of the Sun every second. So there is 3.8 x joules of energy being produced in the core of the Sun every second. Remember that the nuclear reactions are what is producing this energy. So the next thing we should figure out is how many reactions are occurring every second in the core.
12 To do this we need to become Albert Einstein for a few minutes. Mass of a proton (Hydrogen nuclei) = x kg. In the reaction, four protons are changed into one Helium atom. Mass of 4 protons = x kg. Mass of Helium nuclei = x kg. There is less mass in the Helium atom: x kg The missing mass is turned directly into energy. E = mc 2 E = (0.048 x kg)(3.0 x 10 8 m/s) 2 E = 4.32 x joules for every reaction
13 So now we know how much energy is produced for each nuclear reaction: 4.32 x joules/reaction We also know that the core produces 3.8 x joules/second How do we find out the number of reactions/second?
14 30 How do you find out reactions/second? x J/reaction divided by 3.8 x J/second x J/reaction multiplied by 3.8 x J/second x J/second divided by 4.32 x J/reaction 60 0% 0% 0%
15 Reaction/second = (3.8 x J/second)/ (4.32 x J/reaction) So there are 8.8 x reactions/second occurring in the Sun. The Sun converts 564 million tons of hydrogen into 560 million tons of helium every second. That means that every second 4 million tons of hydrogen is turned into energy. ON the order of one Mount Everest per second.
16 So now we know how fast we are burning our fuel. But the last thing we need to know is how big the fuel tank is. In an earlier class we calculated the mass of the Sun using Kepler s third law. It comes out to be Mass = 2 x kg. The mass of the Sun s core, where the reactions are occurring is about 10% of the total Sun s mass. M core = 2 x kg. We want to use this value to discover how many reactions can occur in the Sun.
17 Remember that it takes 4 hydrogen nuclei to make one helium. So for one reaction to occur, we need the mass of four hydrogen atoms. We found that earlier. Mass of 4 protons = x kg. or we could say that there is x kg/reaction We know that M core = 2 x kg. So how do we find the total number of reactions possible in the Sun?
18 30 How do we find the total number of possible reactions in the Sun? 1. (2 x kg) divided by x kg/reaction 2. (6.692 x kg/reaction ) divided by 2 x kg 3. 2 x kg multiplied by x kg/reaction % 0% 0%
19 Total # of reactions = (2 x kg.)/(6.692 x kg/reaction) Total # of reactions = 3 x reactions Now we are almost finished. We know the total number of reactions that are possible 3 x reactions (the amount of fuel) And we know the rate of the reactions 8.8 x reactions/second (rate of consumption) How can you now, figure out how long the Sun s lifetime is?
20 5 How can we figure out the Sun s lifetime? 1. 3 x reactions multiplied by 8.8 x reactions/second 2. 3 x reactions divided by 8.8 x reactions/second x reactions/second divided by 3 x reactions 45 0% 0% 0%
21 Lifetime of Sun = (3 x reactions)/(8.8 x reactions/second) Lifetime of Sun = 3.4 X seconds Since there are π x 10 7 seconds in a year. Lifetime of Sun = 10.8 billion years. More precise calculations find the lifetime to be more like 10 billion years. The Sun is currently about 4.6 billion years old. We have another 5 billion years until the fuel runs out.
22 There are only two assumptions made in this model #1. The Sun is not shrinking or expanding. This means that the emitted luminosity is equal to the energy being produced in the core every second. #2. The luminosity of the Sun has not changed over its lifetime. The rate of consumption is constant. #1 appears to be true from observations, and #2 seems to be true because temperatures have been very stable on Earth for at least 3 billion years.
Objectives 404 CHAPTER 9 RADIATION
Objectives Explain the difference between isotopes of the same element. Describe the force that holds nucleons together. Explain the relationship between mass and energy according to Einstein s theory
Solar Energy Production
Solar Energy Production We re now ready to address the very important question: What makes the Sun shine? Why is this such an important topic in astronomy? As humans, we see in the visible part of the
Physics 1104 Midterm 2 Review: Solutions
Physics 114 Midterm 2 Review: Solutions These review sheets cover only selected topics from the chemical and nuclear energy chapters and are not meant to be a comprehensive review. Topics covered in these
Basics of Nuclear Physics and Fission
Basics of Nuclear Physics and Fission A basic background in nuclear physics for those who want to start at the beginning. Some of the terms used in this factsheet can be found in IEER s on-line glossary.
The Sun and Solar Energy
I The Sun and Solar Energy One of the most important forces behind global change on Earth is over 90 million miles distant from the planet. The Sun is the ultimate, original source of the energy that drives
Multiple Choice Identify the choice that best completes the statement or answers the question.
Test 2 f14 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Carbon cycles through the Earth system. During photosynthesis, carbon is a. released from wood
AS COMPETITION PAPER 2007 SOLUTIONS
AS COMPETITION PAPER 2007 Total Mark/50 SOLUTIONS Section A: Multiple Choice 1. C 2. D 3. B 4. B 5. B 6. A 7. A 8. C 1 Section B: Written Answer Question 9. A mass M is attached to the end of a horizontal
The Sun. Solar radiation (Sun Earth-Relationships) The Sun. The Sun. Our Sun
The Sun Solar Factoids (I) The sun, a medium-size star in the milky way galaxy, consisting of about 300 billion stars. (Sun Earth-Relationships) A gaseous sphere of radius about 695 500 km (about 109 times
Stellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
Lesson 6: Earth and the Moon
Lesson 6: Earth and the Moon Reading Assignment Chapter 7.1: Overall Structure of Planet Earth Chapter 7.3: Earth s Interior More Precisely 7-2: Radioactive Dating Chapter 7.5: Earth s Magnetosphere Chapter
Particle Soup: Big Bang Nucleosynthesis
Name: Partner(s): Lab #7 Particle Soup: Big Bang Nucleosynthesis Purpose The student explores how helium was made in the Big Bang. Introduction Very little helium is made in stars. Yet the universe is
Why Does the Sun Shine?
Why Does the Sun Shine? Is the Sun on Fire? Fire (oxidation) produces light and heat, just like the Sun. Source: chemical potential energy Suppose the Sun were made of carbon and oxygen. The Sun could
Work and Energy. Work = Force Distance. Work increases the energy of an object. Energy can be converted back to work.
Work and Energy Ch. 6 Work = Force Distance Work increases the energy of an object. Energy can be converted back to work. Therefore, energy and work have the same unit: Newton meter = Nm Energy per gram,
Structure and Properties of Atoms
PS-2.1 Compare the subatomic particles (protons, neutrons, electrons) of an atom with regard to mass, location, and charge, and explain how these particles affect the properties of an atom (including identity,
WHERE DID ALL THE ELEMENTS COME FROM??
WHERE DID ALL THE ELEMENTS COME FROM?? In the very beginning, both space and time were created in the Big Bang. It happened 13.7 billion years ago. Afterwards, the universe was a very hot, expanding soup
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Chapter 5: #50 Hotter Sun: Suppose the surface temperature of the Sun were about 12,000K, rather than 6000K. a. How
Lecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
Energy and Energy Resources
CHAPTER 9 DIRECTED READING WORKSHEET Energy and Energy Resources As you read Chapter 9, which begins on page 212 of your textbook, answer the following questions. Strange but True! (p. 212) 1. What vast
Atomic Calculations. 2.1 Composition of the Atom. number of protons + number of neutrons = mass number
2.1 Composition of the Atom Atomic Calculations number of protons + number of neutrons = mass number number of neutrons = mass number - number of protons number of protons = number of electrons IF positive
The Deepwater Horizon Oil Spill Part I. Unit Conversion
The Deepwater Horizon Oil Spill Part I. Unit Conversion Why? The Deepwater Horizon oil spill (also known as the BP oil spill) began on 4/20/2010 and ended when the well was capped on 7/15/2010. The spill
Name Class Period. F = G m 1 m 2 d 2. G =6.67 x 10-11 Nm 2 /kg 2
Gravitational Forces 13.1 Newton s Law of Universal Gravity Newton discovered that gravity is universal. Everything pulls on everything else in the universe in a way that involves only mass and distance.
Chapter 18: The Structure of the Atom
Chapter 18: The Structure of the Atom 1. For most elements, an atom has A. no neutrons in the nucleus. B. more protons than electrons. C. less neutrons than electrons. D. just as many electrons as protons.
Light as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
Buoyancy and Archimedes Principle. Buoyancy and Archimedes Principle Assume block is in equilibrium.
Assume block is in equilibrium. Then upward forces must equal downward forces. Upward force: pressure from fluid Downward force: atmospheric pressure plus weight Therefore In this case, the object is less
Chemistry 1000 Lecture 2: Nuclear reactions and radiation. Marc R. Roussel
Chemistry 1000 Lecture 2: Nuclear reactions and radiation Marc R. Roussel Nuclear reactions Ordinary chemical reactions do not involve the nuclei, so we can balance these reactions by making sure that
A i A i. µ(ion) = Z i X i
Lecture 2 Review: calculation of mean atomic weight of an ionized gas (µ) Given a mass fraction X i (or abundance) for an ionic (or atomic) species with atomic weight A i, we can can calculate µ by: For
Objectives. PAM1014 Introduction to Radiation Physics. Constituents of Atoms. Atoms. Atoms. Atoms. Basic Atomic Theory
PAM1014 Introduction to Radiation Physics Basic Atomic Theory Objectives Introduce and Molecules The periodic Table Electronic Energy Levels Atomic excitation & de-excitation Ionisation Molecules Constituents
In science, energy is the ability to do work. Work is done when a force causes an
What is energy? In science, energy is the ability to do work. Work is done when a force causes an object to move in the direction of the force. Energy is expressed in units of joules (J). A joule is calculated
Photons. ConcepTest 27.1. 1) red light 2) yellow light 3) green light 4) blue light 5) all have the same energy. Which has more energy, a photon of:
ConcepTest 27.1 Photons Which has more energy, a photon of: 1) red light 2) yellow light 3) green light 4) blue light 5) all have the same energy 400 nm 500 nm 600 nm 700 nm ConcepTest 27.1 Photons Which
Origins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
Astro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
18.2 Comparing Atoms. Atomic number. Chapter 18
As you know, some substances are made up of only one kind of atom and these substances are called elements. You already know something about a number of elements you ve heard of hydrogen, helium, silver,
Introduction to Nuclear Physics
Introduction to Nuclear Physics 1. Atomic Structure and the Periodic Table According to the Bohr-Rutherford model of the atom, also called the solar system model, the atom consists of a central nucleus
MASS DEFECT AND BINDING ENERGY
MASS DEFECT AND BINDING ENERGY The separate laws of Conservation of Mass and Conservation of Energy are not applied strictly on the nuclear level. It is possible to convert between mass and energy. Instead
Beginning of the Universe Classwork 6 th Grade PSI Science
Beginning of the Universe Classwork Name: 6 th Grade PSI Science 1 4 2 5 6 3 7 Down: 1. Edwin discovered that galaxies are spreading apart. 2. This theory explains how the Universe was flattened. 3. All
UNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
Chapter Test B. Chapter: Measurements and Calculations
Assessment Chapter Test B Chapter: Measurements and Calculations PART I In the space provided, write the letter of the term or phrase that best completes each statement or best answers each question. 1.
right, left, back total air quality in exhaust air channel (ventilator free flow m_/h
Miami Sun Technical Data Bodyline model: MS 4500.6 27 x 160 W 18 x 160 W 6 x 400 W total power input in watt (with air conditioning) 11800 (13050) CEE 20 A weight in kg gross / net 400/360 model: MS 450.6
1.1 A Modern View of the Universe" Our goals for learning: What is our place in the universe?"
Chapter 1 Our Place in the Universe 1.1 A Modern View of the Universe What is our place in the universe? What is our place in the universe? How did we come to be? How can we know what the universe was
Science Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
2 The Structure of Atoms
CHAPTER 4 2 The Structure of Atoms SECTION Atoms KEY IDEAS As you read this section, keep these questions in mind: What do atoms of the same element have in common? What are isotopes? How is an element
7. In which part of the electromagnetic spectrum are molecules most easily detected? A. visible light B. radio waves C. X rays D.
1. Most interstellar matter is too cold to be observed optically. Its radiation can be detected in which part of the electromagnetic spectrum? A. gamma ray B. ultraviolet C. infrared D. X ray 2. The space
circular motion & gravitation physics 111N
circular motion & gravitation physics 111N uniform circular motion an object moving around a circle at a constant rate must have an acceleration always perpendicular to the velocity (else the speed would
5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
A. 81 2 = 6561 times greater. B. 81 times greater. C. equally strong. D. 1/81 as great. E. (1/81) 2 = 1/6561 as great.
Q12.1 The mass of the Moon is 1/81 of the mass of the Earth. Compared to the gravitational force that the Earth exerts on the Moon, the gravitational force that the Moon exerts on the Earth is A. 81 2
2. Orbits. FER-Zagreb, Satellite communication systems 2011/12
2. Orbits Topics Orbit types Kepler and Newton laws Coverage area Influence of Earth 1 Orbit types According to inclination angle Equatorial Polar Inclinational orbit According to shape Circular orbit
The Universe Inside of You: Where do the atoms in your body come from?
The Universe Inside of You: Where do the atoms in your body come from? Matthew Mumpower University of Notre Dame Thursday June 27th 2013 Nucleosynthesis nu cle o syn the sis The formation of new atomic
Forms of Energy: Multiple Transformations : Teacher Notes
Forms of Energy: Multiple Transformations : Teacher Notes Introduction The focus of the investigation is to further define energy and realize that chains of energy transformations can occur. The VoltageCurrent,
Energy What is Energy? Energy is the ability to do work. Any object that has energy has the ability to create force. Energy is one of the fundamental building blocks of our universe. Energy appears in
1. In the general symbol cleus, which of the three letters. 2. What is the mass number of an alpha particle?
1. In the general symbol cleus, which of the three letters Z A X for a nu represents the atomic number? 2. What is the mass number of an alpha particle? 3. What is the mass number of a beta particle? 4.
Name: Date: Period: Gravity Study Guide
Vocabulary: Define the following terms. Law of Universal Gravitation Gravity Study Guide Weight Weightlessness Gravitational Field Black hole Escape velocity Math: Be able to use the equation for the law
ch 15 practice test Multiple Choice Identify the letter of the choice that best completes the statement or answers the question.
ch 15 practice test Multiple Choice Identify the letter of the choice that best completes the statement or answers the question. 1. Work is a transfer of a. energy. c. mass. b. force. d. motion. 2. What
Newton s Laws of Motion
Newton s Laws of Motion The Earth revolves around the sun in an elliptical orbit. The moon orbits the Earth in the same way. But what keeps the Earth and the moon in orbit? Why don t they just fly off
Chapter 6. Work and Energy
Chapter 6 Work and Energy The concept of forces acting on a mass (one object) is intimately related to the concept of ENERGY production or storage. A mass accelerated to a non-zero speed carries energy
Name: Earth 110 Exploration of the Solar System Assignment 1: Celestial Motions and Forces Due in class Tuesday, Jan. 20, 2015
Name: Earth 110 Exploration of the Solar System Assignment 1: Celestial Motions and Forces Due in class Tuesday, Jan. 20, 2015 Why are celestial motions and forces important? They explain the world around
Instructors Guide: Atoms and Their Isotopes
Instructors Guide: Atoms and Their Isotopes Standards Connections Connections to NSTA Standards for Science Teacher Preparation C.3.a.1 Fundamental structures of atoms and molecules. C.3.b.27 Applications
Chapter 2: Forms of Energy
Chapter 2: Forms of Energy Goals of Period 2 Section 2.1: To describe the forms of energy Section 2.2: To illustrate conversions from one form of energy to another Section 2.3: To define the efficiency
This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
The Sun: Our nearest star
The Sun: Our nearest star Property Surface T Central T Luminosity Mass Lifetime (ms) Value 5500K 15x10 6 K 2 x 10 33 ergs 4 x 10 33 grams 10 billion years Solar Structure Build a model and find the central
Energy efficiency and fuel consumption of fuel cells powered test railway vehicle
Energy efficiency and fuel consumption of fuel cells powered test railway vehicle K.Ogawa, T.Yamamoto, T.Yoneyama Railway Technical Research Institute, TOKYO, JAPAN 1. Abstract For the purpose of an environmental
Astronomy 110 Homework #04 Assigned: 02/06/2007 Due: 02/13/2007. Name:
Astronomy 110 Homework #04 Assigned: 02/06/2007 Due: 02/13/2007 Name: Directions: Listed below are twenty (20) multiple-choice questions based on the material covered by the lectures this past week. Choose
Work, Energy and Power
Name: KEY Work, Energy and Power Objectives: 1. To understand work and its relation to energy. 2. To understand how energy can be transformed from one form into another. 3. To compute the power from the
What Is Energy? Energy and Work: Working Together. 124 Chapter 5 Energy and Energy Resources
1 What You Will Learn Explain the relationship between energy and work. Compare kinetic and potential energy. Describe the different forms of energy. Vocabulary energy kinetic energy potential energy mechanical
Masses in Atomic Units
Nuclear Composition - the forces binding protons and neutrons in the nucleus are much stronger (binding energy of MeV) than the forces binding electrons to the atom (binding energy of ev) - the constituents
Gravitational Potential Energy
Gravitational Potential Energy Consider a ball falling from a height of y 0 =h to the floor at height y=0. A net force of gravity has been acting on the ball as it drops. So the total work done on the
Basic Nuclear Concepts
Section 7: In this section, we present a basic description of atomic nuclei, the stored energy contained within them, their occurrence and stability Basic Nuclear Concepts EARLY DISCOVERIES [see also Section
Practice final for Basic Physics spring 2005 answers on the last page Name: Date:
Practice final for Basic Physics spring 2005 answers on the last page Name: Date: 1. A 12 ohm resistor and a 24 ohm resistor are connected in series in a circuit with a 6.0 volt battery. Assuming negligible
9/13/2013. However, Dalton thought that an atom was just a tiny sphere with no internal parts. This is sometimes referred to as the cannonball model.
John Dalton was an English scientist who lived in the early 1800s. Dalton s atomic theory served as a model for how matter worked. The principles of Dalton s atomic theory are: 1. Elements are made of
Nuclear Physics. Nuclear Physics comprises the study of:
Nuclear Physics Nuclear Physics comprises the study of: The general properties of nuclei The particles contained in the nucleus The interaction between these particles Radioactivity and nuclear reactions
Blackbody radiation. Main Laws. Brightness temperature. 1. Concepts of a blackbody and thermodynamical equilibrium.
Lecture 4 lackbody radiation. Main Laws. rightness temperature. Objectives: 1. Concepts of a blackbody, thermodynamical equilibrium, and local thermodynamical equilibrium.. Main laws: lackbody emission:
Energy Quiz. Questions:
Energy Quiz Want to have some fun and learn at the same time. This is not a test. You don t have to pass it and it won t give you a grade. It will just help you learn or find out how much you remember
Using Photometric Data to Derive an HR Diagram for a Star Cluster
Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and
Review 1. Multiple Choice Identify the choice that best completes the statement or answers the question.
Review 1 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. When hydrogen nuclei fuse into helium nuclei a. the nuclei die. c. particles collide. b. energy
13- What is the maximum number of electrons that can occupy the subshell 3d? a) 1 b) 3 c) 5 d) 2
Assignment 06 A 1- What is the energy in joules of an electron undergoing a transition from n = 3 to n = 5 in a Bohr hydrogen atom? a) -3.48 x 10-17 J b) 2.18 x 10-19 J c) 1.55 x 10-19 J d) -2.56 x 10-19
Name Class Date. You do twice as much work. b. You lift two identical books one meter above the ground.
Exercises 9.1 Work (pages 145 146) 1. Circle the letter next to the correct mathematical equation for work. work = force distance work = distance force c. work = force distance d. work = force distance
Teaching Time: One-to-two 50-minute periods
Lesson Summary Students create a planet using a computer game and change features of the planet to increase or decrease the planet s temperature. Students will explore some of the same principles scientists
Stellar Evolution. The Basic Scheme
Stellar Evolution The Basic Scheme Stars live for a very long time compared to human lifetimes. Even though stellar life-spans are enormous, we know how stars are born, live, and die. All stars follow
CHAPTER 2 Energy Fundamentals for Energy Auditors
CHAPTER 2 Energy Fundamentals for Energy Auditors What is Energy? 2 Energy Lets Us Do Work Energy is the ability to do work. As such, energy is important to all living things in order to maintain life
The University of the State of New York REGENTS HIGH SCHOOL EXAMINATION PHYSICAL SETTING PHYSICS. Wednesday, June 17, 2015 1:15 to 4:15 p.m.
P.S./PHYSICS The University of the State of New York REGENTS HIGH SCHOOL EXAMINATION PHYSICAL SETTING PHYSICS Wednesday, June 17, 2015 1:15 to 4:15 p.m., only The possession or use of any communications
Chapter 3 Review Math 1030
Section A.1: Three Ways of Using Percentages Using percentages We can use percentages in three different ways: To express a fraction of something. For example, A total of 10, 000 newspaper employees, 2.6%
Chapter 1 Student Reading
Chapter 1 Student Reading Chemistry is the study of matter You could say that chemistry is the science that studies all the stuff in the entire world. A more scientific term for stuff is matter. So chemistry
TEACHER BACKGROUND INFORMATION THERMAL ENERGY
TEACHER BACKGROUND INFORMATION THERMAL ENERGY In general, when an object performs work on another object, it does not transfer all of its energy to that object. Some of the energy is lost as heat due to
The Earth, Sun, and Moon
reflect The Sun and Moon are Earth s constant companions. We bask in the Sun s heat and light. It provides Earth s energy, and life could not exist without it. We rely on the Moon to light dark nights.
Science Tutorial TEK 6.9C: Energy Forms & Conversions
Name: Teacher: Pd. Date: Science Tutorial TEK 6.9C: Energy Forms & Conversions TEK 6.9C: Demonstrate energy transformations such as energy in a flashlight battery changes from chemical energy to electrical
Work and Conservation of Energy
Work and Conservation of Energy Topics Covered: 1. The definition of work in physics. 2. The concept of potential energy 3. The concept of kinetic energy 4. Conservation of Energy General Remarks: Two
= 800 kg/m 3 (note that old units cancel out) 4.184 J 1000 g = 4184 J/kg o C
Units and Dimensions Basic properties such as length, mass, time and temperature that can be measured are called dimensions. Any quantity that can be measured has a value and a unit associated with it.
MCQ - ENERGY and CLIMATE
1 MCQ - ENERGY and CLIMATE 1. The volume of a given mass of water at a temperature of T 1 is V 1. The volume increases to V 2 at temperature T 2. The coefficient of volume expansion of water may be calculated
Modeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
Elements of Physics Motion, Force, and Gravity Teacher s Guide
Teacher s Guide Grade Level: 9 12 Curriculum Focus: Physical Science Lesson Duration: Three class periods Program Description Examine Isaac Newton's laws of motion, the four fundamental forces of the universe,
As you learned in the previous activity, energy is either potential energy or kinetic energy. Each can take many forms.
Topic 6: Forms of Potential Energy As you learned in the previous activity, energy is either potential energy or kinetic energy. Each can take many forms. Forms of potential energy include Stored Mechanical
Atomic Structure: Chapter Problems
Atomic Structure: Chapter Problems Bohr Model Class Work 1. Describe the nuclear model of the atom. 2. Explain the problems with the nuclear model of the atom. 3. According to Niels Bohr, what does n stand
Radiation Transfer in Environmental Science
Radiation Transfer in Environmental Science with emphasis on aquatic and vegetation canopy media Autumn 2008 Prof. Emmanuel Boss, Dr. Eyal Rotenberg Introduction Radiation in Environmental sciences Most
Negative Exponents and Scientific Notation
3.2 Negative Exponents and Scientific Notation 3.2 OBJECTIVES. Evaluate expressions involving zero or a negative exponent 2. Simplify expressions involving zero or a negative exponent 3. Write a decimal
Unit 3.2: The Periodic Table and Periodic Trends Notes
Unit 3.2: The Periodic Table and Periodic Trends Notes The Organization of the Periodic Table Dmitri Mendeleev was the first to organize the elements by their periodic properties. In 1871 he arranged the
Composition of the Atmosphere. Outline Atmospheric Composition Nitrogen and Oxygen Lightning Homework
Molecules of the Atmosphere The present atmosphere consists mainly of molecular nitrogen (N2) and molecular oxygen (O2) but it has dramatically changed in composition from the beginning of the solar system.
Atoms and Elements. Outline Atoms Orbitals and Energy Levels Periodic Properties Homework
Atoms and the Periodic Table The very hot early universe was a plasma with cationic nuclei separated from negatively charged electrons. Plasmas exist today where the energy of the particles is very high,
Chemistry 2 Chapter 13: Electrons in Atoms Please do not write on the test Use an answer sheet! 1 point/problem 45 points total
Chemistry 2 Chapter 13: Electrons in Atoms Please do not write on the test Use an answer sheet! 1 point/problem 45 points total 1. Calculate the energy in joules of a photon of red light that has a frequency
PROTONS AND ELECTRONS
reflect Imagine that you have a bowl of oranges, bananas, pineapples, berries, pears, and watermelon. How do you identify each piece of fruit? Most likely, you are familiar with the characteristics of
How Big is Our Solar System?
How Big is Our Solar System? 1.1 Our solar system is so big it is almost impossible to imagine its size if you use ordinary units like feet or miles. The distance from Earth to the Sun is 93 million miles