Chapter 13 The Transfer of Heat.

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Presentation transcript:

Chapter 13 The Transfer of Heat

Convection is the process in which heat is carried from one place to another by the bulk movement of a fluid. convection currents

Conduction is the process whereby heat is transferred directly through a material, with any bulk motion of the material playing no role in the transfer. One mechanism for conduction occurs when the atoms or molecules in a hotter part of the material vibrate or move with greater energy than those in a cooler part. By means of collisions, the more energetic molecules pass on some of their energy to their less energetic neighbors. Materials that conduct heat well are called thermal conductors, and those that conduct heat poorly are called thermal insulators.

The amount of heat Q that is conducted through the bar depends on 13.2 Conduction The amount of heat Q that is conducted through the bar depends on a number of factors: The time during which conduction takes place. The temperature difference between the ends of the bar. The cross sectional area of the bar. The length of the bar.

CONDUCTION OF HEAT THROUGH A MATERIAL The heat Q conducted during a time t through a bar of length L and cross-sectional area A is thermal conductivity SI Units of Thermal Conductivity: J/(s·m·Co)

13.2 Conduction

Materials with dead air spaces are usually excellent thermal 13.2 Conduction Materials with dead air spaces are usually excellent thermal insulators.

Radiation is the process in which energy is transferred by means of electromagnetic waves. A material that is a good absorber is also a good emitter. A material that absorbs completely is called a perfect blackbody.

THE STEFAN-BOLTZMANN LAW OF RADIATION The emissivity e is a dimensionless number between zero and one. It is the ratio of what an object radiates to what the object would radiate if it were a perfect emitter. THE STEFAN-BOLTZMANN LAW OF RADIATION The radiant energy Q, emitted in a time t by an object that has a Kelvin temperature T, a surface area A, and an emissivity e, is given by Stefan-Boltzmann constant

Example 6 A Super-giant Star 13.3 Radiation Example 6 A Super-giant Star The super-giant star has a surface temperature of about 2900 K and emits a power of approximately 4x1030W. Assuming that super-giant is a perfect emitter and spherical, find its radius.

13.3 Radiation