Quantum Physics III (8.06) Spring 2008 Solution Set 1
|
|
- April Fitzgerald
- 5 years ago
- Views:
Transcription
1 Quantum Physics III (8.06) Spring 2008 Solution Set 1 February 12, Natural Units (a) (4 points) In cgs units we have the numbers a, b, c giving the dimensions of Q as [Q] = [gm] a [cm] b [s] c. (1) Using equation (2) from the Problem Set we can directly write [s] = [ ][ev ] 1, [cm] = [c][ ][ev ] 1, [gm] = [ev ][c] 2. (2) Inserting these into (1) we obtain α = b 2a β = b + c γ = a b c (3) One can also invert the above expressions to get a = β + γ, b = α + 2β + 2γ, c = α β 2γ (4) (b) (10 points) Below, we specify the values of a, b, c according to (1) and then calculate α, β, γ according to (3) [force]: The dimensions of force can be read from Newton s second law as [force] =[mass][acceleration] =[mass][length][time] 2. This gives a = 1, b = 1, c = 2 = α = 1, β = 1 γ = 2 = [force] = [c] 1 [ ] 1 [ev ] 2 [pressure]: The dimensions of pressure can be read from its definition [pressure] =[force]/[area] =[gm][cm] 1 [sec] 2. This gives a = 1, b = 1, c = 2 = α = 3, β = 3 γ = 4 = [pressure] = [c] 3 [ ] 3 [ev ] 4 1
2 [conductivity]: Conductivity for free electrons is given by ne 2 τ/m, where n is the number of electrons per unit volume, e is the electron charge, τ is the relaxation time and m is the electron mass. In order to find the units of conductivity we first need to find the units of charge in cgs. Using the Coulomb force law in cgs (F = q 1 q 2 /r 2, q 1,2 =charge, r=distance between charges), we find [charge] = [gm] 1/2 [cm] 3/2 [sec] 1. (5) Using the expression for the conductivity of free electrons given above we find [conductivity]=[sec] 1 and hence [conductivity] = [ ] 1 [ev ]. [magnetic moment]: The magnetic moment has dimension of [Energy]/[magnetic field]. Using the expression for the Lorentz force, F = q(v/c)b, we find [B]=[gm] 1/2 [cm] 1/2 [sec] 1 and hence [magnetic moment] = [c] 3/2 [ ] 3/2 [ev ] 1. [Note: If one uses the definition µ = IA where I is current and A is area, one would get an extra factor c for the unit for magnetic moment compared with the above answer. The difference is due to the choice of unit for magnetic field B. Full credit for this answer.] [viscosity]: Using the definition given in the Problem Set for viscosity we find [viscosity] =[gm][cm] 1 [sec] 1 = [viscosity] = [c] 3 [ ] 2 [ev ] 3 2. Planck scales (a) (3 points) In cgs and natural units, [G N ] = [gm] 1 [cm] 3 [s] 1 = [c] 5 [ ][ev ] 2. This gives [ev ] = [c] 5/2 [ ] 1/2 [G N ] 1/2. Hence using the results from problem 1 we can construct Notice that this allows us to express M P l =, (6) G N GN l P l = c 3, (7) GN t P l = c 5, (8) G N = M 2 P l (9) (b) (5 points) In natural units G N = GeV 2 5. Using (6) M P l = GeV c 2. In cgs units, M P l = gm. 2
3 The compton wavelength of a Planck mass particle is M P l c = GN c 3 = l P l. (10) t P l = l P l /c that is light travels a distance l P l in time t P l. In cgs units l P l = cm and t P l = s. (c) (4 points) m e = 0.511MeV/c 2 and the compton wavelength for the electron is λ e = /m e c. Then (taking positive values) E grav m e c 2 = G N m 2 e/λ e m e c 2 = G Nm 2 e = ( me M P l Thus for electrons, the gravitational effect is very small. (d) (3 points) E grav M P l c 2 = G NMP 2 l /l P l M P l c 2 = G NM 2 P l ) 2 = (11) = 1. (12) The above equation implies that for a Plank mass particle gravity becomes strong at a distance scale of its own Compton wavelength. Thus in understanding the quantum mechanical behavior of such a particle, one can no longer ignore the gravitational effects. In other words, one needs quantum gravity. [Note: full credit if h is used instead of in various expressions above.] 3. The Accelerating Universe (a) (3 points) The cosmological constant has units of energy density. The natural scale for the cosmological constant Λ is thus M Plank /lplank 3. M Plank and l Plank are the natural scales of mass and length in the unit system of, c and G N, which are M P l = G N GN l P l = We can now find the natural value of Λ: c 3 M P l /lp ev l = cm 3 (b) (2 point) In Planck units, the observed value is Λ = , which is an extremely tiny number. 4. Fermi energy, velocity and temperature of copper (a) (2 points) The Fermy energy of copper is E F = 2 2m (3ρπ2 ) 2/3 3
4 where ρ is the number of free electrons per unit volume. For copper there is one free electron per atom, therefore ρ = N Ad A 8.96 gm/cm atoms = = atoms/cm gm/mole mole where N A is the Avogadro s number, d is the density of copper and A is the atomic weight of copper. Substituting numbers we obtain (b) (2 points) E F 7.1eV erg. The corresponding Fermi velocity can be found from the relationship E F = 1 2 mv2 F. We have 2EF v F = m = c = c = cm/sec Since the Fermi velocity is much smaller than the speed of light we can safely assume that electrons in the copper crystal are nonrelativistic. Note that the obtained Fermi v F velocity is about c/137, i.e. is of order of e 2 /, the electron velocity in hydrogen atom. This agrees with what one expects on dimensional grounds. (c) (2 points) The Fermi temperature is given by T F = E F k B K 7.1eV. Therefore we can approximate the electron gas to be at zero temperature. (d) (2 points) The degeneracy pressure is P = (3π2 ) m ρ gm cm sec atm. 5. Free fermion gas in two dimensional well (6 points) Let the size of the square well be a, the number of electrons be N and the Fermi wavevector be denoted as k F. Following similar steps as the calculation done in class for a 3-dimensional fermion gas: (spin degeneracy) (area in k-space)/(area per point in k-space) = number of electrons = πkf 2 ( π a )2 = N, (13) where the factor of 2 comes from the spin degeneracy and the factor of 1/4 comes from requirement that we only count positive wavevectors (in 2 dimensions this becomes a restriction to the first quadrant in k x -k y space). Denoting the electron number density as σ = N/a 2, we find k F = (2πσ) 1/2. (14) 4
5 The Fermi energy is given by where m e is the electron mass. E F = 2 k 2 F 2m e = 2 πσ m e, (15) 6. White dwarfs, Neutron stars and Black holes (6 points) In this problem we treat the star in a constant density approximation ignoring selfconsistency which leads to a more complicated density profile. In parts a and b we assume the particles are nonrelativistic. (a) (3 points) Note: The derivation of the gravitational energy and the energy of a degenerate electron gas was done in class. The total energy was found to be: where E tot = k 2N 2 R + k 1N 5/3 R 2 k 1 = 3 2 f 5/3 10m e ( ) 2/3 9π, k 2 = 3G Nm 2 p. (16) 4 5 The white dwarf s radius is obtained by minimizing the total energy with respect to R, resulting to R white dwarf = 2k 1 k 2 N 1/3 = 7150 km. This is in fact very close to Earth s radius (a coincidence of course). The ratio of the mass densities of the white dwarf and the sun is ( ) 3 ρ white dwarf R Sun = = ρ Sun R white dwarf (b) In a neutron star the pressure is so great that the electrons have merged with protons to form neutrons, so we may assume that the star consists entirely from neutrons. The formula (16) holds if we replace m e with m p and use f = 1. The radius of the neutron star with the mass of the sun is R neutron star = 12.3 km. The neutron Fermi energy is E F = 2 k 2 F 2m = 2 2mR 2 ( 9πfM 4m p ) 2/3. To find if the neutrons in the neutron star should be treated as relativistic particles we calculate the ration of the Fermi energy to the rest energy of the neutron E F m p c 2 = 0.06, 5
6 thus the neutrons are nonrelativistic. Note: Consider a black hole of mass M. The quantity MG N c 2 has dimensions of length. Since it is the only quantity with the dimension of length which can be constructed out of G N,M and c it should therefore equal to the Schwarzschild radius, r s, up to a numerical constant (any object lyingwithin this radius from the center of gravity of the black hole cannotescape and will be devoured by the hole, this defines the surface of no return ). For a star with mass equal to the mass of the Sun, we can estimate r s MG N c km. 7. Free electron gas (a) (4 points) Here, we will treat the electrons as a gas inside a box of volume V and try to estimate when the Coulomb interactions between the electrons become important. The average volume per electron is V/N e. We can ignore the Coulomb interactions if per electron E degeneracy E Coulomb. (17) The energy of a degenerate electron gas was calculated in class and it was found to be An estimate of the Coulomb energy is given by E degeneracy = 3 2 kf 2. (18) 5 2m e E Coulomb e2 r e 2 e 2 ( ) 1/3 = V (3π 2 ) k 1/3 F, (19) N e where k F = ( ) 3π 2 1/3 Ne V and r is the average distance between electrons. Hence the approximation is valid if 3(3π 2 ) 1/3 10 k F e 2 1. (20) m e c (b) (2 points) As discussed in lecture, for mass equal to the Sun s mass we have k F /m e c 1. Since the numerical prefactor in (20), 3(3π 2 ) 1/3 /10, is also of order 1 and /e 2 137, then inequality (20) is satisfied and we can ignore the Coulomb interactions. Note: For electrons in copper, considered in Problem 4, the left hand side of inequality (20) gives us 0.67 and thus ignoring Coulomb interactions between electrons in copper may be suspect. 6
Please read the following instructions:
MIDTERM #1 PHYS 33 (MODERN PHYSICS II) DATE/TIME: February 16, 17 (8:3 a.m. - 9:45 a.m.) PLACE: RB 11 Only non-programmable calculators are allowed. Name: ID: Please read the following instructions: This
More informationPhysics 607 Final Exam
Physics 67 Final Exam Please be well-organized, and show all significant steps clearly in all problems. You are graded on your work, so please do not just write down answers with no explanation! Do all
More informationASTR 5110 Atomic & Molecular Physics Fall Stat Mech Midterm.
ASTR 5110 Atomic & Molecular Physics Fall 2013. Stat Mech Midterm. This is an open book, take home, 24 hour exam. When you have finished, put your answers in the envelope provided, mark the envelope with
More informationThe energy of this state comes from the dispersion relation:
Homework 6 Solutions Problem 1: Kittel 7-2 a The method is the same as for the nonrelativistic gas. A particle confined in a box of volume L 3 is described by a the set of wavefunctions ψ n sinn x πx/l
More informationk m Figure 1: Long problem L2 2 + L2 3 I 1
LONG PROBLEMS 1: Consider the system shown in Figure 1: Two objects, of mass m 1 and m, can be treated as point-like. Each of them is suspended from the ceiling by a wire of negligible mass, and of length
More informationPlease read the following instructions:
MIDTERM #1 PHYS 33 (MODERN PHYSICS II) DATE/TIME: February 16, 17 (8:3 a.m. - 9:45 a.m.) PLACE: RB 11 Only non-programmable calculators are allowed. Name: ID: Please read the following instructions: This
More informationLecture 15: Electron Degeneracy Pressure
Lecture 15: Electron Degeneracy Pressure As the core contracts during shell H-burning we reach densities where the equation of state becomes significantly modified from that of the ideal gas law. The reason
More informationOrder of Magnitude Estimates in Quantum
Order of Magnitude Estimates in Quantum As our second step in understanding the principles of quantum mechanics, we ll think about some order of magnitude estimates. These are important for the same reason
More informationAPPENDIX 1. THE ATOMIC, NUCLEAR AND BLACK HOLE DENSITIES
7 February 2014 - ore 13.20 APPENDIX 1. THE ATOMIC, NUCLEAR AND BLACK HOLE DENSITIES The Schwarzschild formula remains as it is despite all developments [1] in the physics of Black Holes including what
More informationModern Physics Departmental Exam Last updated November 2013
Modern Physics Departmental Exam Last updated November 213 87 1. Recently, 2 rubidium atoms ( 37 Rb ), which had been compressed to a density of 113 atoms/cm 3, were observed to undergo a Bose-Einstein
More information8.04 Spring 2013 February 13, 2013 Problem 1. (15 points) Radiative collapse of a classical atom
Problem Set 1 Solutions 8.04 Spring 01 February 1, 01 Problem 1. (15 points) Radiative collapse of a classical atom (a) (5 points) We begin by assuming that the orbit is circular. This seems like circular
More informationPHY 140A: Solid State Physics. Solution to Homework #7
PHY 14A: Solid State Physics Solution to Homework #7 Xun Jia 1 December 5, 26 1 Email: jiaxun@physics.ucla.edu Fall 26 Physics 14A c Xun Jia (December 5, 26) Problem #1 Static magnetoconductivity tensor.
More information[variable] = units (or dimension) of variable.
Dimensional Analysis Zoe Wyatt wyatt.zoe@gmail.com with help from Emanuel Malek Understanding units usually makes physics much easier to understand. It also gives a good method of checking if an answer
More informationPotential energy, from Coulomb's law. Potential is spherically symmetric. Therefore, solutions must have form
Lecture 6 Page 1 Atoms L6.P1 Review of hydrogen atom Heavy proton (put at the origin), charge e and much lighter electron, charge -e. Potential energy, from Coulomb's law Potential is spherically symmetric.
More informationElementary particles and typical scales in high energy physics
Elementary particles and typical scales in high energy physics George Jorjadze Free University of Tbilisi Zielona Gora - 23.01.2017 GJ Elementary particles and typical scales in HEP Lecture 1 1/18 Contents
More informationUnits and Magnitudes (lecture notes)
Units and Magnitudes (lecture notes) This lecture has two parts. The first part is mainly a practical guide to the measurement units that dominate the particle physics literature, and culture. The second
More informationUsing that density as the electronic density, we find the following table of information for the requested quantities:
Physics 40 Solutions to Problem Set 11 Problems: Fermi gases! The Pauli Exclusion Principle causes much of the behavior of matter, both of the type you are quite familiar with e.g, the hardness of solids,
More informationPhysics 202. Professor P. Q. Hung. 311B, Physics Building. Physics 202 p. 1/2
Physics 202 p. 1/2 Physics 202 Professor P. Q. Hung 311B, Physics Building Physics 202 p. 2/2 Momentum in Special Classically, the momentum is defined as p = m v = m r t. We also learned that momentum
More informationStellar Evolution ASTR 2110 Sarazin. HR Diagram vs. Mass
Stellar Evolution ASTR 2110 Sarazin HR Diagram vs. Mass Trip to Conference Away on conference in the Netherlands next week. Molly Finn, TA, will be our guest lecturer Stellar Evolution ASTR 2110 Sarazin
More informationLecture 11: Periodic systems and Phonons
Lecture 11: Periodic systems and Phonons Aims: Mainly: Vibrations in a periodic solid Complete the discussion of the electron-gas Astrophysical electrons Degeneracy pressure White dwarf stars Compressibility/bulk
More informationPhysics 4213/5213 Lecture 1
August 28, 2002 1 INTRODUCTION 1 Introduction Physics 4213/5213 Lecture 1 There are four known forces: gravity, electricity and magnetism (E&M), the weak force, and the strong force. Each is responsible
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Final Exam
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Physics 8.282J EAPS 12.402J May 20, 2005 Final Exam Name Last First (please print) 1. Do any
More informationName Final Exam December 14, 2016
Name Final Exam December 14, 016 This test consists of five parts. Please note that in parts II through V, you can skip one question of those offered. Part I: Multiple Choice (mixed new and review questions)
More informationConstants and Conversions
Fundamental constants Constants and Conversions Gravitational constant: G=6.67408 10 8 dyn cm 2 g 2 = 6.67408 10 8 g 1 cm 3 s 2 = 6.67408 10 8 erg cm g 2 = 2.960 10 4 M 1 AU 3 days 2 = 1.327 10 11 M 1
More informationequals the chemical potential µ at T = 0. All the lowest energy states are occupied. Highest occupied state has energy µ. For particles in a box:
5 The Ideal Fermi Gas at Low Temperatures M 5, BS 3-4, KK p83-84) Applications: - Electrons in metal and semi-conductors - Liquid helium 3 - Gas of Potassium 4 atoms at T = 3µk - Electrons in a White Dwarf
More informationFACULTY OF SCIENCE. High Energy Physics. WINTHROP PROFESSOR IAN MCARTHUR and ADJUNCT/PROFESSOR JACKIE DAVIDSON
FACULTY OF SCIENCE High Energy Physics WINTHROP PROFESSOR IAN MCARTHUR and ADJUNCT/PROFESSOR JACKIE DAVIDSON AIM: To explore nature on the smallest length scales we can achieve Current status (10-20 m)
More informationChapter 7 Neutron Stars
Chapter 7 Neutron Stars 7.1 White dwarfs We consider an old star, below the mass necessary for a supernova, that exhausts its fuel and begins to cool and contract. At a sufficiently low temperature the
More informationFree Electron Fermi Gas and Energy Bands
PHYS 353 SOLID STATE PHYSICS STUDY GUIDE FOR PART 3 OUTLINE: Free Electron Fermi Gas and Energy Bands A. Quantum Theory and energy levels 1. Schrodinger's equation 2. quantum numbers and energy levels
More informationGravity, Strings and Branes
Gravity, Strings and Branes Joaquim Gomis International Francqui Chair Inaugural Lecture Leuven, 11 February 2005 Fundamental Forces Strong Weak Electromagnetism QCD Electroweak SM Gravity Standard Model
More informationNeutron Stars. Chapter 14: Neutron Stars and Black Holes. Neutron Stars. What s holding it up? The Lighthouse Model of Pulsars
Neutron Stars Form from a 8-20 M Sun star Chapter 14: Neutron Stars and Black Holes Leftover 1.4-3 M Sun core after supernova Neutron Stars consist entirely of neutrons (no protons) Neutron Star (tennis
More informationLecture notes 9: The end states of stars
Lecture notes 9: The end states of stars We have seen that the two most important properties governing the structure of a star such as the Sun are 1. self gravitation; a star obeying the ideal equation
More informationQuantum mechanics of many-fermion systems
Quantum mechanics of many-fermion systems Kouichi Hagino Tohoku University, Sendai, Japan 1. Identical particles: Fermions and Bosons 2. Simple examples: systems with two identical particles 3. Pauli principle
More informationJanuary 2017 Qualifying Exam
January 2017 Qualifying Exam Part I Calculators are allowed. No reference material may be used. Please clearly mark the problems you have solved and want to be graded. Do only mark the required number
More informationRelativistic Astrophysics Neutron Stars, Black Holes & Grav. W. ... A brief description of the course
Relativistic Astrophysics Neutron Stars, Black Holes & Grav. Waves... A brief description of the course May 2, 2009 Structure of the Course Introduction to General Theory of Relativity (2-3 weeks) Gravitational
More informationFall 2012 Qualifying Exam. Part I
Fall 2012 Qualifying Exam Part I Calculators are allowed. No reference material may be used. Please clearly mark the problems you have solved and want to be graded. Do only mark the required number of
More informationApplied Nuclear Physics (Fall 2006) Lecture 1 (9/6/06) Basic Nuclear Concepts
22.101 Applied Nuclear Physics (Fall 2006) Lecture 1 (9/6/06) Basic Nuclear Concepts References Table of Isotopes, C. M. Lederer and V. S. Shirley, ed. (Wiley & Sons, New York, 1978), 7 th ed. Table of
More informationPHYSICS 250 May 4, Final Exam - Solutions
Name: PHYSICS 250 May 4, 999 Final Exam - Solutions Instructions: Work all problems. You may use a calculator and two pages of notes you may have prepared. There are problems of varying length and difficulty.
More informationNuclear Synthesis. PHYS 162 Lectures 10a,b 1
Nuclear Synthesis All elements heavier than Helium are made inside stars up to Iron - fusion in Red Giants heavier than Iron (and some lighter) - Supernova explosions Stars lose matter at end of life-cycle
More informationEvolution of High Mass stars
Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes
More informationEnergy Wave Equations: Correction Factors
Energy Wave Equations: Correction Factors Jeff Yee jeffsyee@gmail.com March 16, 2018 Summary The equations in Energy Wave Theory accurately model particle energy, photon energy, forces, atomic orbitals
More informationThe Bohr Model of Hydrogen
The Bohr Model of Hydrogen Suppose you wanted to identify and measure the energy high energy photons. One way to do this is to make a calorimeter. The CMS experiment s electromagnetic calorimeter is made
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Quiz 2
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Astronomy 8.282J 12.402J April 13, 2005 Quiz 2 Name Last First (please print) 1. Work any
More informationThe Stellar Black Hole
The Stellar Black Hole Kenneth Dalton e-mail: kxdalton@yahoo.com Abstract A black hole model is proposed in which a neutron star is surrounded by a neutral gas of electrons and positrons. The gas is in
More information(n, l, m l ) 3/2/2016. Quantum Numbers (QN) Plots of Energy Level. Roadmap for Exploring Hydrogen Atom
PHYS 34 Modern Physics Atom III: Angular Momentum and Spin Roadmap for Exploring Hydrogen Atom Today Contents: a) Orbital Angular Momentum and Magnetic Dipole Moment b) Electric Dipole Moment c) Stern
More informationThe Cosmological Constant Problem
Physics 171 Fall 2015 The Cosmological Constant Problem 1 The numerical value of the vacuum energy density The cosmological constant Λ was introduced by Albert Einstein into general relativity in 1917
More informationFinal Exam Practice Solutions
Physics 390 Final Exam Practice Solutions These are a few problems comparable to those you will see on the exam. They were picked from previous exams. I will provide a sheet with useful constants and equations
More informationNewton s law of gravitation in 11 dimensions
Planck Units in 11 Dimensions Mikhail Vlasov 5 Casa Verde Foothill Ranch, CA 92610 vlasovm@hotmail.com September 20, 2011 Abstract Planck units are derived from five physical constants (Gravitational constant,
More informationSolutions Final exam 633
Solutions Final exam 633 S.J. van Enk (Dated: June 9, 2008) (1) [25 points] You have a source that produces pairs of spin-1/2 particles. With probability p they are in the singlet state, ( )/ 2, and with
More informationAST1100 Lecture Notes
AST11 Lecture Notes Part 1G Quantum gases Questions to ponder before the lecture 1. If hydrostatic equilibrium in a star is lost and gravitational forces are stronger than pressure, what will happen with
More informationPHYSICS 219 Homework 2 Due in class, Wednesday May 3. Makeup lectures on Friday May 12 and 19, usual time. Location will be ISB 231 or 235.
PHYSICS 219 Homework 2 Due in class, Wednesday May 3 Note: Makeup lectures on Friday May 12 and 19, usual time. Location will be ISB 231 or 235. No lecture: May 8 (I m away at a meeting) and May 29 (holiday).
More informationWelcome back to Physics 211. Physics 211 Spring 2014 Lecture Gravity
Welcome back to Physics 211 Today s agenda: Newtonian gravity Planetary orbits Gravitational Potential Energy Physics 211 Spring 2014 Lecture 14-1 1 Gravity Before 1687, large amount of data collected
More informationASTR 200 : Lecture 21. Stellar mass Black Holes
1 ASTR 200 : Lecture 21 Stellar mass Black Holes High-mass core collapse Just as there is an upper limit to the mass of a white dwarf (the Chandrasekhar limit), there is an upper limit to the mass of a
More informationTermination of Stars
Termination of Stars Some Quantum Concepts Pauli Exclusion Principle: "Effectively limits the amount of certain kinds of stuff that can be crammed into a given space (particles with personal space ). When
More informationAdvanced Higher Physics
Wallace Hall Academy Physics Department Advanced Higher Physics Quanta Problems AH Physics: Quanta 1 2015 Data Common Physical Quantities QUANTITY SYMBOL VALUE Gravitational acceleration g 9.8 m s -2 Radius
More informationSynergizing Screening Mechanisms on Different Scales
Synergizing Screening Mechanisms on Different Scales Jeremy Sakstein University of Pennsylvania Probing the dark sector and general relativity at all scales CERN 17 th August 2017 Or. What should astrophysical
More informationLecture 11: The Internal Structure of Stars Reading: Section 18-2
Lecture 11: The Internal Structure of Stars Reading: Section 18-2 Key Ideas: Observational Clues to Stellar Structure H-R Diagram Mass-Luminosity Relation Hydrostatic Equilibrium Balance between Gravity
More informationKatsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy
11/14/12 Katsushi Arisaka 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Seven Phases of Cosmic Evolution 11/14/12 Katsushi Arisaka
More informationProtostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium
Protostars on the HR Diagram Once a protostar is hot enough to start, it can blow away the surrounding gas Then it is visible: crosses the on the HR diagram The more the cloud, the it will form stars Lifetimes
More informationNovel Tests of Gravity Using Astrophysics
Novel Tests of Gravity Using Astrophysics Jeremy Sakstein University of Pennsylvania Department of Physics & Astronomy University of Mississippi 1 st November 2016 Some Thoughts on Gravitational Physics
More informationM04M.1 Particles on a Line
Part I Mechanics M04M.1 Particles on a Line M04M.1 Particles on a Line Two elastic spherical particles with masses m and M (m M) are constrained to move along a straight line with an elastically reflecting
More informationSmooth Bang Theory: The Universe Steadily Gains Mass With Rate c 3 /G
Smooth Bang Theory: The Universe Steadily Gains Mass With Rate c 3 /G Abstract Mikhail Vlasov Email: vlasovm@hotmail.com October 31, 2015 According to spectroscopic data of light coming from distant galaxies
More informationUnit III Free Electron Theory Engineering Physics
. Introduction The electron theory of metals aims to explain the structure and properties of solids through their electronic structure. The electron theory is applicable to all solids i.e., both metals
More information3. On cold, dark fall nights, why does frost preferentially form on the horizontal surfaces of cars and not on their vertical surfaces?
Part I 7-Minute Questions 1. A tennis ball of mass m is held just above a basketball of mass M! m and radius R. The bottom of the basketball is held a height h above the ground. With their centers vertically
More informationThe general solution of Schrödinger equation in three dimensions (if V does not depend on time) are solutions of time-independent Schrödinger equation
Lecture 17 Page 1 Lecture 17 L17.P1 Review Schrödinger equation The general solution of Schrödinger equation in three dimensions (if V does not depend on time) is where functions are solutions of time-independent
More informationAnnouncement. Station #2 Stars. The Laws of Physics for Elementary Particles. Lecture 9 Basic Physics
Announcement Pick up your quiz after this lecture as you leave the lecture hall. Homework#2 due on Thursday No hand-written homework! Please staple them! Put it in the box before the lecture begins! Station
More informationMath Questions for the 2011 PhD Qualifier Exam 1. Evaluate the following definite integral 3" 4 where! ( x) is the Dirac! - function. # " 4 [ ( )] dx x 2! cos x 2. Consider the differential equation dx
More informationFundamental Constants
Fundamental Constants Atomic Mass Unit u 1.660 540 2 10 10 27 kg 931.434 32 28 MeV c 2 Avogadro s number N A 6.022 136 7 36 10 23 (g mol) 1 Bohr magneton μ B 9.274 015 4(31) 10-24 J/T Bohr radius a 0 0.529
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 6 Oct. 28, 2015 Today Wrap up of Einstein s General Relativity Curved Spacetime Gravitational Waves Black Holes Relativistic
More informationPHYSICS DEPARTMENT, PRINCETON UNIVERSITY PHYSICS 301 FINAL EXAMINATION. January 13, 2005, 7:30 10:30pm, Jadwin A10 SOLUTIONS
PHYSICS DEPARTMENT, PRINCETON UNIVERSITY PHYSICS 301 FINAL EXAMINATION January 13, 2005, 7:30 10:30pm, Jadwin A10 SOLUTIONS This exam contains five problems. Work any three of the five problems. All problems
More informationName Final Exam December 7, 2015
Name Final Exam December 7, 015 This test consists of five parts. Please note that in parts II through V, you can skip one question of those offered. Part I: Multiple Choice (mixed new and review questions)
More informationLecture 26. High Mass Post Main Sequence Stages
Lecture 26 Fate of Massive Stars Heavy Element Fusion Core Collapse Supernova Neutrinoes Gaseous Remnants Neutron Stars Mar 27, 2006 Astro 100 Lecture 26 1 High Mass Post Main Sequence Stages For M(main
More informationName Solutions to Final Exam December 14, 2016
Name Solutions to Final Exam December 14, 016 This test consists of five parts. Please note that in parts II through V, you can skip one question of those offered. Part I: Multiple Choice (mixed new and
More informationChapter 0 Introduction X-RAY BINARIES
X-RAY BINARIES 1 Structure of this course 0. Introduction 1. Compact stars: formation and observational appearance. Mass transfer in binaries 3. Observational properties of XRBs 4. Formation and evolution
More informationASTR 200 : Lecture 20. Neutron stars
ASTR 200 : Lecture 20 Neutron stars 1 Equation of state: Degenerate matter We saw that electrons exert a `quantum mechanical' pressure. This is because they are 'fermions' and are not allowed to occupy
More informationChapter 2: Equation of State
Introduction Chapter 2: Equation of State The Local Thermodynamic Equilibrium The Distribution Function Black Body Radiation Fermi-Dirac EoS The Complete Degenerate Gas Application to White Dwarfs Temperature
More informationWelcome back to Physics 215
Welcome back to Physics 215 Today s agenda: More rolling without slipping Newtonian gravity Planetary orbits Gravitational Potential Energy Physics 215 Spring 2018 Lecture 13-1 1 Rolling without slipping
More informationNew conceptual foundations for Quantum-Gravity and Quantum-Mechanics
New conceptual foundations for Quantum-Gravity and Quantum-Mechanics B N Sreenath P B No 20,HPO, Shimoga-577201, Karnataka, India. e-mail: bnsreenath@yahoo.co.in Abstract. Quantum-Gravity (QG) is limited
More informationGraduate Written Examination Fall 2014 Part I
Graduate Written Examination Fall 2014 Part I University of Minnesota School of Physics and Astronomy Aug. 19, 2014 Examination Instructions Part 1 of this exam consists of 10 problems of equal weight.
More informationMass-Volume Relation. ( 3 π 2 ) ⅔ ħ 2 Z ρ. π G ρ 2 R 2 = ( 18 π ) ⅔ ħ 2 Z
Mass-Volume Relation Chandrasekhar realized, that there has to be a maximum mass for a white dwarf Equating the central pressure estimate with the electron degeneracy pressure yields 2 3 π G ρ 2 R 2 =
More informationStellar Interiors - Hydrostatic Equilibrium and Ignition on the Main Sequence.
Stellar Interiors - Hydrostatic Equilibrium and Ignition on the Main Sequence http://apod.nasa.gov/apod/astropix.html Outline of today s lecture Hydrostatic equilibrium: balancing gravity and pressure
More informationUNIVERSITY of NORTH CAROLINA at CHAPEL HILL. Doctoral Written Examination in Physics, Part I: Classical mechanics and Statistical mechanics
UNIVERSITY of NORTH CAROLINA at CHAPEL HILL Doctoral Written Examination in Physics, 2012 Part I: Classical mechanics and Statistical mechanics Saturday, May 12, 2012 Instructions: Please work in the assigned
More informationProperties of Elementary Particles
and of Elementary s 01/11/2018 My Office Hours: Thursday 1:00-3:00 PM 212 Keen Building Outline 1 2 3 Consider the world at different scales... Cosmology - only gravity matters XXXXX Input: Mass distributions
More informationProblem 1 Classical Mechanics
Problem 1 Classical Mechanics A pendulum of length l and mass m is attached to a mass M, which is free to move along the axis Ox, as described by the figure. The system is under the influence of a uniform
More informationNuclear mass density in strong gravity and grand unification
Nuclear mass density in strong gravity and grand unification U. V. S. Seshavatharam Honorary faculty, I-SERVE Alakapuri, Hyderabad-5, India e-mail: seshavatharam.uvs@gmail.com Prof. S. Lakshminarayana
More information1 Stellar Energy Generation Physics background
1 Stellar Energy Generation Physics background 1.1 Relevant relativity synopsis We start with a review of some basic relations from special relativity. The mechanical energy E of a particle of rest mass
More information2013 CAP Prize Examination
Canadian Association of Physicists SUPPORTING PHYSICS RESEARCH AND EDUCATION IN CANADA 2013 CAP Prize Examination Compiled by the Department of Physics & Engineering Physics, University of Saskatchewan
More informationChapter 7: Quantum Statistics
Part II: Applications SDSMT, Physics 213 Fall 1 Fermi Gas Fermi-Dirac Distribution, Degenerate Fermi Gas Electrons in Metals 2 Properties at T = K Properties at T = K Total energy of all electrons 3 Properties
More informationLecture 2: Quantum Mechanics and Relativity
Lecture 2: Quantum Mechanics and Relativity Atom Atomic number A Number of protons Z Number of neutrons A-Z Number of electrons Z Charge of electron = charge of proton ~1.6 10-19 C Size of the atom ~10-10
More informationGravity, Strings and Branes
Gravity, Strings and Branes Joaquim Gomis Universitat Barcelona Miami, 23 April 2009 Fundamental Forces Strong Weak Electromagnetism QCD Electroweak SM Gravity Standard Model Basic building blocks, quarks,
More informationSyllabus: Physics 241 Introduction to Modern Physics Professor Marshall Onellion (office)
1 Syllabus: Physics 241 Introduction to Modern Physics Professor Marshall Onellion (office) 263-6829 Office hours: onellion@wisc.edu MW: 10am- 1pm, F: 10am- noon, or by appointment Text: Kenneth Krane,
More informationMethods in Experimental Particle Physics
Methods in Experimental Particle Physics Antonio Di Domenico Dipartimento di Fisica, Sapienza Università di Roma II semester a.y. 2018-2019 (also I semester only this year) 1 Aim of these lectures * *
More informationFree-Fall Timescale of Sun
Free-Fall Timescale of Sun Free-fall timescale: The time it would take a star (or cloud) to collapse to a point if there was no outward pressure to counteract gravity. We can calculate the free-fall timescale
More informationLec 9: Stellar Evolution and DeathBirth and. Why do stars leave main sequence? What conditions are required for elements. Text
1 Astr 102 Lec 9: Stellar Evolution and DeathBirth and Evolution Why do stars leave main sequence? What conditions are required for elements Text besides Hydrogen to fuse, and why? How do stars die: white
More information2. Basic Assumptions for Stellar Atmospheres
2. Basic Assumptions for Stellar Atmospheres 1. geometry, stationarity 2. conservation of momentum, mass 3. conservation of energy 4. Local Thermodynamic Equilibrium 1 1. Geometry Stars as gaseous spheres!
More informationHomework 9 Solution Physics Spring a) We can calculate the chemical potential using eq(6.48): µ = τ (log(n/n Q ) log Z int ) (1) Z int =
Homework 9 Solutions uestion 1 K+K Chater 6, Problem 9 a We can calculate the chemical otential using eq6.48: µ = τ logn/n log Z int 1 Z int = e εint/τ = 1 + e /τ int. states µ = τ log n/n 1 + e /τ b The
More informationAdvanced Higher Physics
Wallace Hall Academy Physics Department Advanced Higher Physics Astrophysics Problems Data Common Physical Quantities QUANTITY SYMBOL VALUE Gravitational acceleration g 9.8 m s -2 Radius of Earth R E 6.4
More informationPhysics 342: Modern Physics
Physics 342: Modern Physics Final Exam (Practice) Relativity: 1) Two LEDs at each end of a meter stick oriented along the x -axis flash simultaneously in their rest frame A. The meter stick is traveling
More informationSeptember 2016 Physics & Astronomy Qualifying Exam for Advancement to Candidacy Day 1: September 1, 2016
September 2016 Physics & Astronomy Qualifying Exam for Advancement to Candidacy Day 1: September 1, 2016 Do not write your name on the exam. Instead, write your student number on each exam booklet. This
More informationAy123 Set 3 solutions
Ay123 Set 3 solutions Mia de los Reyes October 23 218 1. Equation of state and the Chandrasekhar mass (a) Using the Fermi-Dirac distribution for non-relativistic electrons, derive the relationship between
More informationExamination paper for FY2450 Astrophysics
1 Department of Physics Examination paper for FY2450 Astrophysics Academic contact during examination: Rob Hibbins Phone: 94820834 Examination date: 01-06-2015 Examination time: 09:00 13:00 Permitted examination
More information