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UVA - PHYS - 606
University of Virginia Department of PhysicsPhysics 606: How Things Work IILecture #1 Slides: Introduction to course and SkatingQuestion: SkatingA rotary lawn mower spins its sharp blade rapidly over the lawn and cuts the tops of the grasses o
UVA - PHYS - 606
University of Virginia Department of PhysicsPhysics 606: How Things Work IILecture #26 Slides: MicrowavesQuestion:If you put a CD in a microwave oven, it willMicrowave Ovens1. do nothing. 2. burn up the microwave oven. 3. burn up the CD.O
UVA - PHYS - 606
Welcome to the Phys 606 Chat Room 8-9 PM Apr 16 You are free to type text in the text line anytime. If you want to speak, Click on the hand and I will give you the floor. We all should do this just to say hello Then I will review selected topics.
UVA - PHYS - 606
University of Virginia Department of PhysicsPhysics 606: How Things Work IILecture #5 Slides: SeesawsWork Lifting Ball Going straight up: Force is large Distance is smallForces on a RampSupport Net Forcedistancework =force Weight
UVA - CS - 101
Applications of Scientific Computing9. Scientific ComputingScience and engineering challenges.! !Commercial applications.! !!!!!!!!!!Fluid dynamics. Seismic surveys. Plasma dynamics. Ocean circulation. Electronics design.
UVA - CS - 101
Overview4.1 - 4.2 Analysis of AlgorithmsAnalysis of algorithms. Framework for comparing algorithms and predicting performance. Scientific method. Observe some feature of the universe. Hypothesize a model that is consistent with observation. Predi
UVA - CS - 686
Dependable ComputingDependable Computing CS686John C. Knight Department of Computer Science University of Virginia knight@cs.virginia.edu 434.982.2216 John C. Knight, 2009 - All rights reserved.Beginning of Course MemoReadit is on the Web site
UVA - SBB - 801
!" " ) ( )# !$% & % " ( " , % . ( %'" * +""," / (,)( -/ " ) 1 ( 2 * % " ( ( %" " " ( 3 ) ( ( ( (" *( ( 0 % + 4 " ( "*) #5 6$ " " ( % 4( % )/0 ) ( ( ( ( # ! 9 &: " " * ) " / " " / 7 " / 7 ) 89% " ") ' ) (* " $% %
UVA - AE - 554
Components of Galaxies Gas The Importance of Gas Fuel for star formation (H2) Tracer of galaxy kinematics/mass (HI) Tracer of dynamical history of interaction between galaxies (HI)Much of this material has been / will be covered in your ISM
UVA - AST - 554
Components of Galaxies Gas The Importance of Gas Fuel for star formation (H2) Tracer of galaxy kinematics/mass (HI) Tracer of dynamical history of interaction between galaxies (HI)Much of this material has been / will be covered in your ISM
UVA - AE - 554
AST 554 - Homework #1Due February 24, 2009 Note: This homework covers some of the topics in the preliminary lectures up through "Components of Galaxies: Gas". The problems are intended to be relatively straight-forward. Please remember to define al
UVA - AST - 554
AST 554 - Homework #1Due February 24, 2009 Note: This homework covers some of the topics in the preliminary lectures up through "Components of Galaxies: Gas". The problems are intended to be relatively straight-forward. Please remember to define al
UVA - AE - 554
Components of Galaxies: Dark MatterDark Matter: Any Form of matter whose existence is inferred solely through its gravitational effects. -B&T, pg 590 Nature of Major Component of Universe Galaxy Formation Fate of the UniverseEvidence for Dark M
UVA - AST - 554
Components of Galaxies: Dark MatterDark Matter: Any Form of matter whose existence is inferred solely through its gravitational effects. -B&T, pg 590 Nature of Major Component of Universe Galaxy Formation Fate of the UniverseEvidence for Dark M
UVA - AE - 554
The Astrophysical Journal, 686:948965, 2008 October 20# 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A.ATHE RESOLVED PROPERTIES OF EXTRAGALACTIC GIANT MOLECULAR CLOUDSAlberto D. Bolatto,1 Adam K. Leroy,2 Erik Ros
UVA - AST - 554
The Astrophysical Journal, 686:948965, 2008 October 20# 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A.ATHE RESOLVED PROPERTIES OF EXTRAGALACTIC GIANT MOLECULAR CLOUDSAlberto D. Bolatto,1 Adam K. Leroy,2 Erik Ros
UVA - AE - 554
The Astrophysical Journal, 629:6171, 2005 August 10# 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A.THE RELATIONSHIP BETWEEN LUMINOSITY AND BROAD-LINE REGION SIZE IN ACTIVE GALACTIC NUCLEIShai Kaspi,1, 2 Dan Maoz,1
UVA - AST - 554
The Astrophysical Journal, 629:6171, 2005 August 10# 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A.THE RELATIONSHIP BETWEEN LUMINOSITY AND BROAD-LINE REGION SIZE IN ACTIVE GALACTIC NUCLEIShai Kaspi,1, 2 Dan Maoz,1
UVA - AE - 554
THE ASTROPHYSICAL JOURNAL, 507 : 615654, 1998 November 10( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A.ROTATING NUCLEAR RINGS AND EXTREME STARBURSTS IN ULTRALUMINOUS GALAXIES D. DOWNESInstitut de Radio Astronomi
UVA - AST - 554
THE ASTROPHYSICAL JOURNAL, 507 : 615654, 1998 November 10( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A.ROTATING NUCLEAR RINGS AND EXTREME STARBURSTS IN ULTRALUMINOUS GALAXIES D. DOWNESInstitut de Radio Astronomi
UVA - AE - 554
The Astronomical Journal, 124:788810, 2002 August# 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A.MOLECULAR GAS IN ELLIPTICAL GALAXIES: DISTRIBUTION AND KINEMATICS L. M. YoungPhysics Department, New Mexico Institut
UVA - AST - 554
The Astronomical Journal, 124:788810, 2002 August# 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A.MOLECULAR GAS IN ELLIPTICAL GALAXIES: DISTRIBUTION AND KINEMATICS L. M. YoungPhysics Department, New Mexico Institut
UVA - AST - 554
1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.289.766H1997MNRAS.
UVA - AE - 554
1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.34
UVA - AST - 554
1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.343.1D1989ApJ.34
UVA - AST - 554
1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K1995ARA&A.33.581K199
UVA - AE - 554
1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S
UVA - AST - 554
1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S1976ApJ.203.297S
UVA - AE - 554
THE ASTROPHYSICAL JOURNAL, 478 : 144161, 1997 March 20( 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A.THE MOLECULAR INTERSTELLAR MEDIUM IN ULTRALUMINOUS INFRARED GALAXIES P. M. SOLOMONAstronomy Program, State Univ
UVA - AST - 554
THE ASTROPHYSICAL JOURNAL, 478 : 144161, 1997 March 20( 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A.THE MOLECULAR INTERSTELLAR MEDIUM IN ULTRALUMINOUS INFRARED GALAXIES P. M. SOLOMONAstronomy Program, State Univ
UVA - AE - 554
1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S
UVA - AST - 554
1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S1983ApJ.265.148S
UVA - AE - 554
Population Synthesis Models: ColorColor DiagramModelsDataComponents of Galaxies: Dust Is efficient at absorbing UV and optical light, and thus affects the interpretation of the emission at these wavelengths (e.g., stellar population synt
UVA - AST - 554
Population Synthesis Models: ColorColor DiagramModelsDataComponents of Galaxies: Dust Is efficient at absorbing UV and optical light, and thus affects the interpretation of the emission at these wavelengths (e.g., stellar population synt
UVA - AE - 554
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies?(Ref: B&M 5.1, S&G 2.2) Temperature Determines the range over which the radiation is emitted Chemical Composition metallicities Lifetimes Determin
UVA - AST - 554
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies?(Ref: B&M 5.1, S&G 2.2) Temperature Determines the range over which the radiation is emitted Chemical Composition metallicities Lifetimes Determin
UVA - AST - 554
1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S1987ApJ.320.238S
UVA - AST - 554
1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.89D1984ApJ.285.
UVA - AST - 554
1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H1983QJRAS.24.267H198
UVA - AE - 554
Mon. Not. R. Astron. Soc. 315, 115139 (2000)The SCUBA Local Universe Galaxy Survey I. First measurements of the submillimetre luminosity and dust mass functionsLoretta Dunne,1 Stephen Eales,1 Michael Edmunds,1 Rob Ivison,2 Paul Alexander3 and Dav
UVA - AST - 554
Mon. Not. R. Astron. Soc. 315, 115139 (2000)The SCUBA Local Universe Galaxy Survey I. First measurements of the submillimetre luminosity and dust mass functionsLoretta Dunne,1 Stephen Eales,1 Michael Edmunds,1 Rob Ivison,2 Paul Alexander3 and Dav
UVA - AST - 554
1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B1978ApJ.224.132B
UVA - AE - 554
1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y199
UVA - AST - 554
1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y1991ARA&A.29.581Y199
UVA - AST - 554
1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.1825B1981AJ.86.18
UVA - PHYS - 356
Phys 356Instructions:Final ExamMay 2, 2007This is an in-class, three hour exam. You may refer to your textbook, class notes, and homework solutions, and you may use a calculator. No other reference materials are permitted. Turn in your solutio
UVA - PHYS - 831
Assignment 33.1 A spherical liquid drop floats in equilibrium with its saturated vapor. The drop has radius r and surface tension , assumed constant. (a) Find the pressure difference between the liquid inside the drop and the saturated vapor. Assume
UVA - PHYS - 831
Assignment 11.1 A gasoline engine uses an approximation to the Otto cycle, in which an ideal gas with initial pressure, volume, and temperature (P1 , V1 , T1 ) is first adiabatically compressed to volume V2 , then heated at constant volume to temper
UVA - PHYS - 831
Thermodynamic VariablesGeneralized forcesPressure Surface tension Tension Magnetic field Electric field Chemical potential Temperature PGeneralized displacementsJ H E Volume Area Length Magnetization Polarization Number Entropy V A L M P N S
UVA - PHYS - 831
Physics 831 Statistical Mechanics ISpring 2009Phys 831 Statistical Mechanics I is a graduate level course in the theories of thermodynamics and statistical mechanics. We will discuss the foundations and relationships of both theories, and survey
UVA - PHYS - 831
Assignment 22.1 Prove that for xed N , (a) E X (b) E Y (c) T dS = CX T Y dY + CYX=Y TTY TX=TTX T+YYX Y T XTdXY2.2 Take N xed throughout this problem. (a) By equating two dierent expressions for dE, show that T dS = CV dT + T
UVA - PHYS - 521
Assignment 85.2 Foucault gyrocompass A gyroscope in the form of a symmetric top is mounted with no gravitaional torque, and its symmetry axis is constrained to move only in the horizontal plane parallel to the earth's surface. The gyroscope is set s
UVA - PHYS - 521
Assignment 95.3 A tilted coin (a sharp-edged uniform disk) of radius a and mass M rolls without slipping on a horizontal plane in a circle of radius b. A set of orthogonal coordinate axes has its origin at the center of ^ ^ mass, with e3 perpendicul
UVA - PHYS - 521
Assignment 62.1 Larmor's Theorem (a) The Lorentz force implies the equation of motion m = e(E + c-1 v B). Prove that the effect of a r weak uniform magnetic field B on the motion of a charged particle in a central electric field E = E(|r|)^ can r b
UVA - PHYS - 521
Assignment 126.8 I went through 6.7 in class on 11/29, so you shouldnt have too much trouble here. For the rotation part, set up the initial coordinates q as spherical (or cylindrical) coordinates with axis along n. Then determine how n L is rel
UVA - PHYS - 356
Phys 356Instructions:Final ExamMay 9, 2008This is an in-class, three hour exam. You may refer to your textbook, class notes, and homework solutions, and you may use a calculator. No other reference materials are permitted. Turn in your solutio
UVA - PHYS - 831
Manipulating DifferentialsA differential relation dF = Adx + Bdy contains a great deal of information, and can be manipulated much like an algebraic relation. For instance, the following derivations are valid: (a) Set dy = 0 and divide by dx: F = A.
UVA - PHYS - 521
Assignment 21.12 The orbit of the planet mercury has an eccentricity of 0.206 and a period of 0.241 year; moreover, the perihelion advances slowly at a rate of 43 seconds of arc per century. One possible explanation of this effect is that the potent
UVA - PHYS - 521
Assignment 106.4 The relativistic motion of a particle in a static potential V (r) can be obtained from the lagrangian L = -mc2 (1 - v 2 /c2 )1/2 - V (r). (a) Write out Lagrange's equations and verify the above assertion. (b) Find the canonical mome
UVA - PHYS - 521
Assignment 11.2 A uniform spool of mass M and diameter d rests on end on a frictionless table. A massless string wrapped around the spool is attached to a weight m which hangs over the edge of the table. If the spool is released from rest when its c