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All condensed matter (solids, liquids, and dense gases) emit electromagnetic radiation at all temperatures. Also, this radiation has a continuous distribution of several wavelengths with different intensities. This is caused by oscillating atoms and molecules and their interaction with the neighbours. In the early nineteenth century, it was established that each element is associated with a characteristic spectrum of radiation, known as Atomic Spectra. Hence, this suggests an intimate relationship between the internal structure of an atom and the spectrum emitted by it.
Atomic Spectra
When an atomic gas or vapour is excited under low pressure by passing an electric current through it, the spectrum of the emitted radiation has specific wavelengths. It is important to note that, such a spectrum consists of bright lines on a dark background. This is an emission line spectrum. Here is an emission line spectrum of hydrogen gas:
Emission lines in the spectrum of hydrogen
The emission line spectra work as a ‘fingerprint’ for identification of the gas. Also, on passing a white light through the gas, the transmitted light shows some dark lines in the spectrum. These lines correspond to those wavelengths that are found in the emission line spectra of the gas. This is the absorption spectrum of the material of the gas.
Normally, one would expect to find a regular pattern in the frequencies of light emitted by a particular element. Let’s look at hydrogen as an example. Interestingly, at the first glance, it is difficult to find any regularity or order in the atomic spectra. However, on close observation, it can be seen that the spacing between lines within certain sets decreases in a regular manner. Each of these sets is a spectral series.
Five spectral series identified in hydrogen are
Further, let’s look at the Balmer series in detail.
1. Balmer SeriesBalmer series in the emission spectrum of hydrogen In 1885, when Johann Balmer observed a spectral series in the visible spectrum of hydrogen, he made the following observations:
Further, for n=∞, you can get the limit of the series at a wavelength of 364.6 nm. Also, you can’t see any lines beyond this; only a faint continuous spectrum. Furthermore, like the Balmer’s formula, here are the formulae for the other series:
2. Lyman Series
where λ is the wavelength
R is the Rydberg's constant and
n can have any integral value.
3. Paschen Series
where λ is the wavelength
R is the Rydberg's constant and
n can have any integral value
4. Brackett Series
where λ is the wavelength
R is the Rydberg's constant and
n can have any integral value
5. Pfund Series
where λ is the wavelength
R is the Rydberg's constant and
n can have any integral value
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