The temperature of a lava flow can be estimated by observing its color

Slides:



Advertisements
Similar presentations
An Introduction to Quantum
Advertisements

Happyphysics.com Physics Lecture Resources Prof. Mineesh Gulati Head-Physics Wing Happy Model Hr. Sec. School, Udhampur, J&K Website: happyphysics.com.
Kirchoff’s Loop Theorem
2. The Particle-like Properties Of Electromagnetic Radiation
Radiation Heat Transfer
The dual nature of light l wave theory of light explains most phenomena involving light: propagation in straight line reflection refraction superposition,
Black body radiation and ultraviolet catastrophe
Lecture 28 — The Planck Distribution Chapter 8, Monday March 24 th Before Planck: Wien and Rayleigh-Jeans The ultraviolet catastrophe The Planck distribution.
What are the 3 ways heat can be transferred? Radiation: transfer by electromagnetic waves. Conduction: transfer by molecular collisions. Convection: transfer.
Introduction to Quantum Physics
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,
Classical vs Quantum Mechanics Rutherford’s model of the atom: electrons orbiting around a dense, massive positive nucleus Expected to be able to use classical.
Black Body radiation Hot filament glows.
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,
The birth of quantum mechanics Until nearly the close of the 19 th century, classical mechanics and classical electrodynamics had been largely successful.
PHY 102: Waves & Quanta Topic 11 EM Radiation from atoms John Cockburn Room E15)
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.
Lecture 1 Quantization of energy. Quantization of energy Energies are discrete (“quantized”) and not continuous. This quantization principle cannot be.
Laws of Radiation Heat Transfer P M V Subbarao Associate Professor Mechanical Engineering Department IIT Delhi Macro Description of highly complex Wave.
Chapter 1 Thermal radiation and Planck’s postulate
Ch 9 pages Lecture 18 – Quantization of energy.
Blackbody Radiation & Atomic Spectra. “Light” – From gamma-rays to radio waves The vast majority of information we have about astronomical objects comes.
 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.
Average Lifetime Atoms stay in an excited level only for a short time (about 10-8 [sec]), and then they return to a lower energy level by spontaneous emission.
The Particlelike Properties of Electromagnetics Radiation Wei-Li Chen 10/27/2014.
Quantum Mechanics. Planck’s Law A blackbody is a hypothetical body which absorbs radiation perfectly for every wave length. The radiation law of Rayleigh-Jeans.
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.
Physics 1C Lecture 28A. Blackbody Radiation Any object emits EM radiation (thermal radiation). A blackbody is any body that is a perfect absorber or emitter.
Radiation Fundamental Concepts EGR 4345 Heat Transfer.
Quantum Theory I An Overview. Introduction The development of classical physics (based on Newton’s laws) culminated in James Clerk Maxwell’s equations:
1 PHYS 3313 – Section 001 Lecture #9 Wednesday, Feb. 12, 2014 Dr. Jaehoon Yu Determination of Electron Charge Line Spectra Blackbody Radiation Wednesday,
Lecture 27 — The Planck Distribution Chapter 8, Friday March 21 st Quick review of exam 2 Black-body radiation Before Planck: Wien and Rayleigh-Jeans The.
4: Introduction to Quantum Physics
Lecture_02: Outline Thermal Emission
Radiation Heat Transfer
Dualisme Cahaya Sebagai Gelombang dan Partikel
Light is a Particle Physics 12.
Blackbody. Kirchhoff’s Radiation  Radiated electromagnetic energy is the source of radiated thermal energy. Depends on wavelengthDepends on wavelength.
Introduction to Physics and Astronomy (1) 2-1. Light and Black Body Radiation.
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
Electromagnetic Radiation Principles
Plan for Today (AP Physics 2) Questions on HW (due tomorrow) Notes/Lecture on Blackbody Radiation.
Basic Science in Remote Sensing
Still have a few registered iclickers (3 or 4
PHYS 3313 – Section 001 Lecture #9
The Planck Distribution
PHYS 3313 – Section 001 Lecture #10

Radiation Process and Properties
General Physics (PHY 2140) Lecture 27 Modern Physics Quantum Physics
Electromagnetic Radiation
Understand the electromagnetic spectrum and how it is organized.
Topic- Black-Body Radation Laws
Early Quantum Theory and Models of the Atom
Black Body Radiation Mr. Sonaji V. Gayakwad Asst. professor
Blackbody Radiation All bodies at a temperature T emit and absorb thermal electromagnetic radiation Blackbody radiation In thermal equilibrium, the power.
Chapter 27 Early Quantum Theory
QM2 Concept Test 8.1 The total energy for distinguishable particles in a three dimensional harmonic oscillator potential
Introduction and Basic Concepts
Blackbody Radiation All bodies at a temperature T emit and absorb thermal electromagnetic radiation Blackbody radiation In thermal equilibrium, the power.
Understand the electromagnetic spectrum and how it is organized.
Electromagnetic Radiation
Section 1: Light and Quantized Energy
PHYS 3313 – Section 001 Lecture #10
RADIATION LAWS.
Presentation transcript:

The temperature of a lava flow can be estimated by observing its color The temperature of a lava flow can be estimated by observing its color. The result agrees well with measured temperatures of lava flows at about 1,000 to 1,200 °C (1,832 to 2,192 °F)

http://phet.colorado.edu/sims/blackbody-spectrum/blackbody-spectrum_en.html

Black body radiation curves showing peak wavelengths at various temperatures

curve behavior. (Classical approach) Rayleigh-Jeans Law: First Attempt to explain Radiation curve behavior. (Classical approach) Rayleigh and Jeans considered the radiation inside the black body (cavity) to be a series of standing electromagnetic waves, on the assumption that the em-wave radiation spectrum emitted by a black body continuously vary in wavelengths from zero to infinity The number of standing waves per unit volume (density of em standing waves or allowed modes or density of states) is This equation is independent of shape of the cavity. λ is wavelength, v is frequency and c is speed of light.

1/Tut9 Calculate the number of allowed modes per unit volume in the wavelength range between 100 nm to 100.2 nm in an enclosure of volume 100 cm3.

curve behavior. (Classical approach) Rayleigh-Jeans Law: First Attempt to explain Radiation curve behavior. (Classical approach)

Ultraviolet catastrophe Let us consider Rayleigh-Jeans formula According to this equation, as ν increases u(ν)dν increases as ν2, and in the limit ν → , u(ν)dν → . However, in reality as shown in the figure, as ν → , u(ν)dν → 0. This discrepancy between theory and the experiment is known as “Ultraviolet catastrophe”.

curve behavior. (analogy to gas molecules) Wein’s Law: Second Attempt to explain Radiation curve behavior. (analogy to gas molecules)

E=nh where n=0, 1,2,3,... E=h Max Planck: blackbody radiation is produced by vibrating submicroscopic electric charges, which he called resonators the walls of a cavity are composed of resonators vibrating at different frequency. Classical Maxwell theory: An oscillator of frequency  could have any value of energy and could change its amplitude continuously by radiating any fraction of its energy Planck: the total energy of a resonator with frequency  could only be an integer multiple of h. (During emission or absorption of light) resonator can change its energy only by the quantum of energy ΔE=h 4h 3h 2h h A black body radiation chamber is filled up not only with radiation, but also with simple harmonic oscillators or resonators (energy emitters) of the molecular dimensions, known as Planck's oscillators or Planck's resonators, which can vibrate, with all possible frequencies. The vibration of the resonator entails one degree of freedom only. The oscillators (or resonators) cannot radiate or absorb energy continuously, but energy is emitted or absorbed in the form of packets or quanta called photons. Planck assumed that each photon has an energy hv where h is the Planck's constant, its value being equal to 6.625  10-34 Joule-sec, and v is the frequency of radiation. This assumption is the most revolutionary in character. In other words, the theory states that the exchange of energy between radiation and matter cannot take place continuously but only in certain multiples of the fundamental frequency of the resonator (energy emitter).As the energy of a photon is hv, the energy emitted (or absorbed) is equal to 0, hv, 2hv, 3hv, ..........nhv, i.e., in multiplets of some small unit, called as quantum. E=nh where n=0, 1,2,3,... E=h

Therefore, the energy density belonging to the range dv can be obtained by multiplying the average energy of Planck's oscillator by the number of oscillators per unit volume, in this frequency range  and ( + dv). where u()d is energy density (i.e., total energy per unit volume) belonging to the range dv called Planck's radiation law in terms of frequency.

"Blackbody radiation" or "cavity radiation" refers to an object or system which absorbs all radiation incident upon it and re-radiates energy which is characteristic of this radiating system only, not dependent upon the type of radiation which is incident upon it. The radiated energy can be considered to be produced by standing wave or resonant modes of the cavity which is radiating

Boltzmann constant = 1.3806503 × 10-23 m2 kg s-2 K-1 Fig.: Comparison of Planck’s formula with Rayleigh-Jeans formula and Wein’s law.

Wien’s displacement law The wavelength whose energy density is greatest can be obtained by setting and solving for λ = λmax. We find Which may be written as This equation is known as Wien’s displacement law. It quantitatively expresses the empirical fact that the peak in the black body spectrum shifts progressively to shorter wavelength (higher frequencies) as the temperature is increased.

Wien’s displacement law

Stefan-Boltzmann Law This equation is known as Stefan-Boltzmann Law. Total energy density within the cavity can be obtained by integrating energy density (eq. 3) over all frequencies. Thus Here a is a universal constant. According to the equation, the total energy density is proportional to the fourth power of the absolute temperature of the cavity walls. Therefore we expect that energy E radiated by a black body per second per unit area is also proportional to T4 i.e. Where, e = emissivity, ranges from 0 (for perfectly reflecting surface) to 1 (for a black body, and σ (Stefan’s constant) =5.67x10-8 watt/m2-K4. This equation is known as Stefan-Boltzmann Law.