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More Precisely 2.1: The Kelvin Temperature Scale

More Precisely 2.1: The Kelvin Temperature Scale

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2.4 Thermal Radiation







Radiation laws:



1.



Peak wavelength is inversely

proportional to temperature.



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2.4 Thermal Radiation







Radiation laws:



2.



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Total energy emitted is proportional to fourth power of temperature.



2.5 Spectroscopy







Spectroscope: Splits light into component colors



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2.5 Spectroscopy







Emission lines: Single frequencies emitted by particular atoms



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2.5 Spectroscopy







The emission spectrum can be used to identify elements.



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2.5 Spectroscopy







Absorption spectrum: If a continuous spectrum passes through a cool gas, atoms of the

gas will absorb the same frequencies they emit.



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2.5 Spectroscopy







Absorption spectrum of the Sun



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2.5 Spectroscopy







Kirchhoff’s laws:











Luminous solid, liquid, or dense gas produces continuous spectrum.

Low-density hot gas produces emission spectrum.

Continuous spectrum incident on cool, thin gas produces absorption spectrum.



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2.5 Spectroscopy







Kirchhoff’s laws illustrated



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2.6 Formation of Spectral Lines







The existence of spectral lines required new model of atom, so that only certain amounts

of energy could be emitted or absorbed.







The Bohr model had certain, allowed orbits for electron.



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2.6 Formation of Spectral Lines









Emission energies correspond to energy differences between allowed levels.

The modern model has electron “cloud” rather than orbit.



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More Precisely 2.1: The Kelvin Temperature Scale

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