To recognize the partnership in between atomic spectra and also the electronic framework of atoms.

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The idea of the photon emerged from testing through thermal radiation, electromagnetic radiation emitted as the outcome of a source’s temperature, which produces a continuous spectrum of energies.The photoelectric result gave indisputable evidence for the visibility of the photon and therefore the particle-favor behavior of electromagnetic radiation. However, more direct proof was essential to verify the quantized nature of power in all issue. In this section, we explain just how monitoring of the interaction of atoms through visible light gave this evidence.


Line Spectra

Although objects at high temperature emit a continuous spectrum of electromagnetic radiation, a different type of spectrum is oboffered when pure samples of individual aspects are heated. For instance, once a high-voltage electrical discharge is passed through a sample of hydrogen gas at low push, the resulting individual isolated hydrogen atoms caused by the dissociation of H2 emit a red light. Unchoose blackbody radiation, the shade of the light emitted by the hydrogen atoms does not depend greatly on the temperature of the gas in the tube. When the emitted light is passed with a prism, only a few narrow lines of specific wavelengths, dubbed a line spectrum, are oboffered quite than a consistent variety of wavelengths (Figure (PageIndex1)). The light emitted by hydrogen atoms is red because, of its 4 characteristic lines, the the majority of intense line in its spectrum is in the red percentage of the visible spectrum, at 656 nm. With sodium, but, we observe a yellow shade bereason the most intense lines in its spectrum are in the yellow percentage of the spectrum, at around 589 nm.

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Figure (PageIndex1): The Emission of Light by Hydrogen Atoms. (a) A sample of excited hydrogen atoms emits a characteristic red light. (CC BY-SA 3.0 Unported; Science Made Aliveby means of Wikipedia)(b) When the light emitted by a sample of excited hydrogen atoms is separation right into its component wavelengths by a prism, four characteristic violet, blue, green, and red emission lines can be observed, the the majority of intense of which is at 656 nm. (CC BY-SA 3.0;Jan Homannusing Wikipedia)

Such emission spectra were observed for many kind of other facets in the late 1ninth century, which presented a significant difficulty because timeless physics was unable to describe them. Part of the explanation is provided by Planck’s equation: the observation of only a couple of values of λ (or ( u )) in the line spectrum supposed that just a couple of values of E were feasible. Therefore the power levels of a hydrogen atom had actually to be quantized; in various other words, just says that had certain values of energy were feasible, or allowed. If a hydrogen atom could have actually any worth of power, then a continuous spectrum would certainly have actually been oboffered, equivalent to blackbody radiation.

In 1885, a Swiss math teacher, Johann Balmer (1825–1898), showed that the frequencies of the lines observed in the visible area of the spectrum of hydrogen fit a straightforward equation that can be expressed as follows:

< u=constant; left ( dfrac12^2-dfrac1n^^2 appropriate ) label6.3.1>

wbelow n = 3, 4, 5, 6. As an outcome, these lines are recognized as the Balmer series. The Swedish physicist Johannes Rydberg (1854–1919) subsequently redeclared and also increased Balmer’s cause the Rydberg equation:

< dfrac1lambda =Re; left ( dfrac1n^2_1-dfrac1n^2_2 ideal ) label6.3.2>

wbelow (n_1) and (n_2) are positive integers, (n_2 > n_1), and also ( Re ) the Rydberg constant, has a worth of 1.09737 × 107 m−1.


Johann Balmer (1825–1898)

A math teacher at a secondary college for girls in Switzerland also, Balmer was 60 years old once he composed the paper on the spectral lines of hydrogen that made him well known.

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Balmer published only one other paper on the topic, which appeared once he was 72 years old.

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Like Balmer’s equation, Rydberg’s straightforward equation described the wavelengths of the visible lines in the emission spectrum of hydrogen (with n1 = 2, n2 = 3, 4, 5,…). More vital, Rydberg’s equation likewise predicted the wavelengths of various other series of lines that would certainly be oboffered in the emission spectrum of hydrogen: one in the ultraviolet (n1 = 1, n2 = 2, 3, 4,…) and one in the infrared (n1 = 3, n2 = 4, 5, 6). Unfortunately, researchers had not yet occurred any kind of theoretical justification for an equation of this form.