Thermo & Stat Mech - Spring 2006 Class 21 1 Thermodynamics and Statistical Mechanics Blackbody Radiation.

Slides:



Advertisements
Similar presentations
Statistical Mechanics
Advertisements

Wavelength, Frequency, and Energy Practice Problems
Light Solar System Astronomy Chapter 4. Light & Matter Light tells us about matter Almost all the information we receive from space is in the form of.
Lecture 28 — The Planck Distribution Chapter 8, Monday March 24 th Before Planck: Wien and Rayleigh-Jeans The ultraviolet catastrophe The Planck distribution.
Down The Rabbit Hole: Quantum Physics Lesson 8. Objectives Define a quantum Calculate the energy of a photon Relate photon energy to wavelength and frequency.
Solar Energy On how the Sun emits energy as radiation, and how the Earth receives it.
Phy100: Blackbody radiation
Blackbody radiation Goals: Understand properties of Black body radiation; Black body radiation Radiation power, intensity and angle dependence.
The mathematics of classical mechanics Newton’s Laws of motion: 1) inertia 2) F = ma 3) action:reaction The motion of particle is represented as a differential.
Chapter 45 The Nature of Light. Light Particle (photon) Wave (electromagnetic wave) Interference Diffraction Polarization.
Thermo & Stat Mech - Spring 2006 Class 20 1 Thermodynamics and Statistical Mechanics Heat Capacities.
Thermo & Stat Mech - Spring 2006 Class 14 1 Thermodynamics and Statistical Mechanics Kinetic Theory of Gases.
Light. What is Light? The third form of energy The only thing astronomers study Electromagnetic radiation The thing that our eyes detect How radio works.
Black Body radiation Hot filament glows.
Phy100: Heat transport Three basic forms of thermal heat transport
Thermo & Stat Mech - Spring 2006 Class 22 1 Thermodynamics and Statistical Mechanics Fermi-Dirac Statistics.
Thermo & Stat Mech - Spring 2006 Class 7 1 Thermodynamics and Statistical Mechanics Tds Equations.
Thermo & Stat Mech - Spring 2006 Class 18 1 Thermodynamics and Statistical Mechanics Statistical Distributions.
What is the nature of Part I. The invention of radio? Hertz proves that light is really an electromagnetic wave. Waves could be generated in one circuit,
Thermo & Stat Mech - Spring 2006 Class 19 1 Thermodynamics and Statistical Mechanics Partition Function.
Thermo & Stat Mech - Spring 2006 Class 17 1 Thermodynamics and Statistical Mechanics Entropy.
The birth of quantum mechanics Until nearly the close of the 19 th century, classical mechanics and classical electrodynamics had been largely successful.
Quantum physics. Quantum physics grew out failures of classical physics which found some quantum remedies in the Planck hypothesis and wave-particle duality.
Light as a Particle. Objectives  Define a quantum  Calculate the energy of a photon  Relate photon energy to wavelength and frequency of EMR.
Physics 361 Principles of Modern Physics Lecture 3.
Radiation: Processes and Properties -Basic Principles and Definitions- Chapter 12 Sections 12.1 through 12.3.
 Radiation emitted by hot objects is called thermal radiation.  Recall that the total radiation power emitted is proportional to T 4, where T is the.
Chapter 18 Bose-Einstein Gases Blackbody Radiation 1.The energy loss of a hot body is attributable to the emission of electromagnetic waves from.
Blackbody radiation How does a solid contain thermal energy? Can a vacuum be “hot”, have a temperature? Why does solid glow when it’s hot? Yes its fields.
Chapter 39 Particles Behaving as Waves
Lecture 4a. Blackbody Radiation Energy Spectrum of Blackbody Radiation - Rayleigh-Jeans Law - Rayleigh-Jeans Law - Wien’s Law - Wien’s Law - Stefan-Boltzmann.
Lecture 24. Blackbody Radiation (Ch. 7) Two types of bosons: (a)Composite particles which contain an even number of fermions. These number of these particles.
Holography. Early Quantum Theory and Models of the Atom.
MODERN PHYSICS REVOLUTION  Classical Newtonian Mechanics, Maxwell’s Electrodynamics, Statistical Mechanics proved hugely successful  BUT…at the beginning.
Thompson’s experiment (discovery of electron) + - V + - Physics at the end of XIX Century and Major Discoveries of XX Century.
Baby-Quiz 1.Why are diffraction effects of your eyes more important during the day than at night? 2.Will the converging lens focus blue light or red light.
Photon Statistics Blackbody Radiation 1.The energy loss of a hot body is attributable to the emission of electromagnetic waves from the body. 2.The.
Radiation Fundamental Concepts EGR 4345 Heat Transfer.
© 2010 Pearson Education, Inc. Range of Visible Light Our eyes can see from 400 (blue/purple) to 700 (red) nm. Nm = nanometers = meters Our eyes.
1 PHYS 3313 – Section 001 Lecture #9 Wednesday, Feb. 12, 2014 Dr. Jaehoon Yu Determination of Electron Charge Line Spectra Blackbody Radiation Wednesday,
Blackbody Radiation Astrophysics Lesson 9.
Question 1 1) wavelength 2) frequency 3) period 4) amplitude 5) energy
What is a Spectrum? How much of observed light is high energy radiation and how much is low energy radiation.
Lecture_02: Outline Thermal Emission
Major Concepts of Physics PHY102 – Lecture #  Syracuse University Lecture #8 Do solids emit light? February 11 th Spring 2015 Prof. Liviu Movileanu.
Light is a Particle Physics 12.
Physical basis of the Greenhouse Effect -The “wavelength shift”- 1.Black body radiation, 2.Absorption spectra 3.Conservation of energy Energy & Environment.
Review of the Wien’s Law Review Chapter Color and Temperature in AstronomyNotes for a more complete discussion of the details of this relationship.
Examples A star radiates as a blackbody at a temperature of 1700 K. At what wavelength does the peak of the blackbody spectrum occur? If you were to look.
Electromagnetic Spectrum Chemistry 6(B). Lesson Objectives Explore the electromagnetic spectrum Understand the mathematical relationships between energy,
Blackbody. Kirchhoff’s Radiation  Radiated electromagnetic energy is the source of radiated thermal energy. Depends on wavelengthDepends on wavelength.
Major Concepts of Physics PHY102 – Lecture #  Syracuse University Lecture #10 Do cold solids emit light? February 24 th Spring 2016 Prof. Liviu.
Cool, invisible galactic gas (60 K, f peak in low radio frequencies) Dim, young star (600K, f peak in infrared) The Sun’s surface (6000K, f peak in visible)
CH Explaining a Continuous Spectrum (called a blackbody spectrum)
STATISTICAL MECHANICS PD Dr. Christian Holm PART 5-6 Some special topics, Thermal Radiation, and Plank distribution.
Physical Principles of Remote Sensing: Electromagnetic Radiation
Associate Professor of Physical Chemistry
The temperature of a lava flow can be estimated by observing its color
Lecture 24. Blackbody Radiation (Ch. 7)
Plan for Today (AP Physics 2) Questions on HW (due tomorrow) Notes/Lecture on Blackbody Radiation.
Down The Rabbit Hole: Quantum Physics
Still have a few registered iclickers (3 or 4
PHYS 3313 – Section 001 Lecture #9

Early Quantum Theory and Models of the Atom
Remote Sensing Remote sensing includes techniques to derive information from a site at a known distance from the sensor.1 Remote sensing is the science.
Thermodynamics and Statistical Mechanics
Blackbody Radiation All bodies at a temperature T emit and absorb thermal electromagnetic radiation Blackbody radiation In thermal equilibrium, the power.
QM2 Concept Test 8.1 The total energy for distinguishable particles in a three dimensional harmonic oscillator potential
Quantum mechanics II Winter 2012
Presentation transcript:

Thermo & Stat Mech - Spring 2006 Class 21 1 Thermodynamics and Statistical Mechanics Blackbody Radiation

Thermo & Stat Mech - Spring 2006 Class 212 Classical Energy Equipartition

Thermo & Stat Mech - Spring 2006 Class 213 Classical Energy Equipartition

Thermo & Stat Mech - Spring 2006 Class 214 Classical Energy Equipartition

Thermo & Stat Mech - Spring 2006 Class 215 Quantum Harmonic Oscillator

Thermo & Stat Mech - Spring 2006 Class 216 Energy of EM Waves in a Cavity Calculate the number of standing wave states in the frequency range between  and  + d . Then Bose-Einstein statistics is used to determine the number of photons in each state. With that information the energy can be calculated.

Thermo & Stat Mech - Spring 2006 Class 217 Density of States (Lec 17)

Thermo & Stat Mech - Spring 2006 Class 218 Density of States for Photons

Thermo & Stat Mech - Spring 2006 Class 219 Photon Energy

Thermo & Stat Mech - Spring 2006 Class 2110 Photon Energy

Thermo & Stat Mech - Spring 2006 Class 2111 Graph

Thermo & Stat Mech - Spring 2006 Class 2112 Total Energy Density

Thermo & Stat Mech - Spring 2006 Class 2113 Energy Flux

Thermo & Stat Mech - Spring 2006 Class 2114 Human Eye and the Sun It is often stated in textbooks that the peak sensitivity of the human eye is at the wavelength at which the energy radiated by the sun is maximum.

Thermo & Stat Mech - Spring 2006 Class 2115 Human Eye Peak at 555 nm

Thermo & Stat Mech - Spring 2006 Class 2116 A Problem? The graph of the energy density as a function of frequency, for a blackbody at a temperature of 5800 K, has a maximum at 1.41 eV. Photons of that energy have a wavelength of 879 nm, which is out of the visible spectrum, in the infrared. What is wrong?

Thermo & Stat Mech - Spring 2006 Class 2117 Solution The energy density is plotted as a function of energy, while the eye’s sensitivity is plotted as a function of wavelength. If we plot the energy density as a function of wavelength, its peak does not occur at 879 nm. How can this be?

Thermo & Stat Mech - Spring 2006 Class 2118 Change to Wavelength

Thermo & Stat Mech - Spring 2006 Class 2119 Wavelength Spectrum

Thermo & Stat Mech - Spring 2006 Class 2120 Graph

Thermo & Stat Mech - Spring 2006 Class 2121 Agreement The maximum of the graph for 5800 K, the temperature of the sun’s surface has a maximum at 500 nm, in reasonable agreement with the peak sensitivity of the human eye.

Thermo & Stat Mech - Spring 2006 Class 2122 Wien Displacement Law

Thermo & Stat Mech - Spring 2006 Class 2123 Photon Gas

Thermo & Stat Mech - Spring 2006 Class 2124 Helmholtz Function

Thermo & Stat Mech - Spring 2006 Class 2125 Pressure