Modern Physics

The reflection of light from a black-colored object.

The electromagnetic energy emitted by an object due to its temperature.

The transmission of heat through a vacuum.

The absorption of all light by an object, causing it to appear black.

It reflects all incoming radiation.

It transmits all incoming radiation.

It absorbs all incoming radiation.

It absorbs some and reflects the rest of incoming radiation.

When the object is highly reflective and polished.

When the object is perfectly transparent.

When the object is in thermal equilibrium with its surroundings and has a high emissivity.

When the object is a poor conductor of heat.

The container will only emit radiation and never absorb it.

The container will only absorb radiation and never emit it.

The container will absorb energy from the room until it reaches thermal equilibrium, at which point it will emit energy at the same rate it absorbs it.

The container will continuously absorb more energy than it emits, eventually reaching an infinitely high temperature.

A discrete spectrum with only specific wavelengths.

A continuous spectrum with all wavelengths.

An absorption spectrum with dark lines against a bright background.

An emission spectrum with bright lines against a dark background.

The wavelength at which the blackbody emits the least radiation.

The average wavelength of the emitted radiation.

The wavelength at which the blackbody emits the most radiation.

The total power emitted by the blackbody.

Classical physics correctly predicted the blackbody spectrum at all wavelengths.

Classical physics predicted that a blackbody would emit infinite energy at short wavelengths, which was not observed.

Classical physics only applied to low-temperature blackbodies.

Classical physics did not consider the concept of energy quantization.

0.5 \mum

5.0 \mum

50 \mum

500 \mum

Star A will have a peak wavelength twice as short as Star B.

Star A will have a peak wavelength twice as long as Star B.

Star A and Star B will have the same peak wavelength.

Star A will have a peak wavelength four times as long as Star B.

10,000 K

5,000 K

1,000 K

500 K