class_2_navamathavan_c1_c2_phy101

8/12/2019 Class_2_Navamathavan_C1_C2_PHY101

1/16

Division of Physics

School of Advanced Sciences

[email protected]

Dr. R. Navamathavan

Physics Division

School of Advanced Sciences ( SAS)

Course: Modern Physics

PHY 101

1414--0707--20142014


2/16

Division of Physics


Course: Modern Physics

PHY 101

Electromagnetic Waves

Black Body Radiation

Planck Radiation Formula

OutlineOutline


3/16

Division of Physics


Introduction Black body radiation Limitations of classical theory

Rayleigh Jeans formula Statistical concepts (FD distributions)

Basic idea of quantization Plancks radiation - Compton effect

Experimental verification Dual nature of Electromagnetic radiation

de-Broglie waves - Davision Germer experiment Heissenberguncertainty principle - Schordinger equation (Time independent and

dependent) Particles in a 1D box Eigen values and Eigen functions

- Quantum Mechanical tunneling Scanning electron microscope -

Quantum confinement quantum well Wire Dots Introduction to

nanomaterials Moores law Properties of nanomaterials Carbons

nanotubes- Applications of nanotechnology in sensors

18 hours

Unit - IUnit - I

CAT - 1


4/16

Division of Physics


Unit - IIUnit - II

12 hoursCAT - 2


5/16

Division of Physics


Unit - IIIUnit - III

15 hoursTEE


6/16

Division of Physics


Text BooksText Books


7/16

Division of Physics


ReferencesReferences


8/16

Division of Physics


IntroductionIntroduction

Three Failures of Classical Physics:Three Failures of Classical Physics:1. Blackbody Radiation

2. The Photoelectric Effect

3. The Hydrogen Atom


9/16

Division of Physics


Some experimental facts:

1. The blackbody spectrum depends only on the temperature of the

object, and not on what it is made of. An iron horseshoe, a ceramic

vase, and a piece of charcoal --- all emit the same blackbody

spectrum if their temperatures are the same.

2. As the temperature of an object increases, it emits more blackbodyenergy at all wavelengths.

3. As the temperature of an object increases, the peak wavelength of

the blackbody spectrum becomes shorter (bluer). For example,

blue stars are hotter than red stars.

4. The blackbody spectrum always becomes small at the left-hand

side (the short wavelength, high frequency side).

Black Body RadiationBlack Body Radiation


10/16

Division of Physics


Any object with a temperature above absolute zero emits light at

all wavelengths. If the object is perfectly black (so it doesn't

reflect any light), then the light that comes from it is

called blackbody radiation.

The energy of blackbody radiation is not shared evenly by all

wavelengths of light.

The spectrum of blackbody radiation (below) shows that somewavelengths get more energy than others.



11/16

Division of Physics


Three spectra are shown, for three different temperatures.

(One of the curves is for the surface temperature of the Sun)



12/16

Division of Physics


When you listen to the radio,

watch TV, or cook dinner in a

microwave oven

Electromagnetic WavesElectromagnetic Waves


13/16

Division of Physics


Electromagnetic WavesElectromagnetic Waves

Waves in the electromagnetic

spectrum vary in size from very

long radio waves the size of

buildings, to very short gamma-rayssmaller than the size of the nucleus

of an atom.


14/16

Division of Physics


Electric and Magnetic Fields in EM WavesElectric and Magnetic Fields in EM Waves


15/16

Division of Physics


Interference of Water WavesInterference of Water Waves


16/16

Division of Physics


Origin of Interference PatternOrigin of Interference Pattern

Constructive interference occurs

when the difference in path lengths

from the slits to the screen is , 2,

3and so on

Destructive interference occurs

where the path difference is

/2, 3 /2, 5 /2and so on

class_2_navamathavan_c1_c2_phy101

Documents