Rydberg formula

In atomic physics, the Rydberg formula calculates the wavelengths of a spectral line in many chemical elements. The formula was primarily presented as a generalization of the Balmer series for all atomic electron transitions of hydrogen. It was first empirically stated in 1888 by the Swedish physicist Johannes Rydberg,[1] then theoretically by Niels Bohr in 1913, who used a primitive form of quantum mechanics. The formula directly generalizes the equations used to calculate the wavelengths of the hydrogen spectral series.

Rydberg's formula as it appears in a November 1888 record

History

In 1880, Rydberg worked on a formula describing the relation between the wavelengths in spectral lines of alkali metals. He noticed that lines came in series and he found that he could simplify his calculations using the wavenumber (the number of waves occupying the unit length, equal to 1/λ, the inverse of the wavelength) as his unit of measurement. He plotted the wavenumbers (n) of successive lines in each series against consecutive integers which represented the order of the lines in that particular series. Finding that the resulting curves were similarly shaped, he sought a single function which could generate all of them, when appropriate constants were inserted.

First he tried the formula: ${\displaystyle \textstyle n=n_{0}-{\frac {C_{0}}{m+m'}}}$, where n is the line's wavenumber, n₀ is the series limit, m is the line's ordinal number in the series, m' is a constant different for different series and C₀ is a universal constant. This did not work very well.

Rydberg was trying: ${\displaystyle \textstyle n=n_{0}-{\frac {C_{0}}{\left(m+m'\right)^{2}}}}$ when he became aware of Balmer's formula for the hydrogen spectrum ${\displaystyle \textstyle \lambda ={hm^{2} \over m^{2}-4}}$ In this equation, m is an integer and h is a constant (not to be confused with the later Planck constant).

Rydberg therefore rewrote Balmer's formula in terms of wavenumbers, as ${\displaystyle \textstyle n=n_{0}-{4n_{0} \over m^{2}}}$.

This suggested that the Balmer formula for hydrogen might be a special case with ${\displaystyle \textstyle m'=0}$ and ${\displaystyle {\text{C}}_{0}=4n_{0}}$, where ${\displaystyle \textstyle n_{0}={\frac {1}{h}}}$, the reciprocal of Balmer's constant (this constant h is written B in the Balmer equation article, again to avoid confusion with Planck's constant).

The term ${\displaystyle {\text{C}}_{0}}$ was found to be a universal constant common to all elements, equal to 4/h. This constant is now known as the Rydberg constant, and m′ is known as the quantum defect.

As stressed by Niels Bohr,[2] expressing results in terms of wavenumber, not wavelength, was the key to Rydberg's discovery. The fundamental role of wavenumbers was also emphasized by the Rydberg-Ritz combination principle of 1908. The fundamental reason for this lies in quantum mechanics. Light's wavenumber is proportional to frequency ${\displaystyle \textstyle {\frac {1}{\lambda }}={\frac {f}{c}}}$, and therefore also proportional to light's quantum energy E. Thus, ${\displaystyle \textstyle {\frac {1}{\lambda }}={\frac {E}{hc}}}$. Modern understanding is that Rydberg's findings were a reflection of the underlying simplicity of the behavior of spectral lines, in terms of fixed (quantized) energy differences between electron orbitals in atoms. Rydberg's 1888 classical expression for the form of the spectral series was not accompanied by a physical explanation. Ritz's pre-quantum 1908 explanation for the mechanism underlying the spectral series was that atomic electrons behaved like magnets and that the magnets could vibrate with respect to the atomic nucleus (at least temporarily) to produce electromagnetic radiation,[3] but this theory was superseded in 1913 by Niels Bohr's model of the atom.

In Bohr's conception of the atom, the integer Rydberg (and Balmer) n numbers represent electron orbitals at different integral distances from the atom. A frequency (or spectral energy) emitted in a transition from n₁ to n₂ therefore represents the photon energy emitted or absorbed when an electron makes a jump from orbital 1 to orbital 2.

Later models found that the values for n₁ and n₂ corresponded to the principal quantum numbers of the two orbitals.

For hydrogen

${\displaystyle {\frac {1}{\lambda _{\mathrm {vac} }}}=R_{\text{H}}\left({\frac {1}{n_{1}^{2}}}-{\frac {1}{n_{2}^{2}}}\right),}$

where

${\displaystyle \lambda _{\mathrm {vac} }}$ is the wavelength of electromagnetic radiation emitted in vacuum,

${\displaystyle R_{\text{H}}}$ is the Rydberg constant for hydrogen, approximately 1.09677583×10⁷ m⁻¹,

${\displaystyle n_{1}}$ is the principal quantum number of an energy level, and

${\displaystyle n_{2}}$ is the principal quantum number of an energy level for the atomic electron transition.

Note:- Here, ${\displaystyle n_{2}}$ > ${\displaystyle n_{1}}$

By setting ${\displaystyle n_{1}}$ to 1 and letting ${\displaystyle n_{2}}$ run from 2 to infinity, the spectral lines known as the Lyman series converging to 91 nm are obtained, in the same manner:

n1	n2	Name	Converge toward
1	2 – ∞	Lyman series	91.13 nm (UV)
2	3 – ∞	Balmer series	364.51 nm (Visible)
3	4 – ∞	Paschen series	820.14 nm (IR)
4	5 – ∞	Brackett series	1458.03 nm (Far IR)
5	6 – ∞	Pfund series	2278.17 nm (Far IR)
6	7 – ∞	Humphreys series	3280.56 nm (Far IR)

A visual comparison of the hydrogen spectral series for n₁ = 1 to n₁ = 6 on a log scale

For any hydrogen-like element

The formula above can be extended for use with any hydrogen-like chemical elements with

${\displaystyle {\frac {1}{\lambda }}=RZ^{2}\left({\frac {1}{n_{1}^{2}}}-{\frac {1}{n_{2}^{2}}}\right),}$

where

${\displaystyle \lambda }$ is the wavelength (in vacuum) of the light emitted,

${\displaystyle R}$ is the Rydberg constant for this element,

${\displaystyle Z}$ is the atomic number, i.e. the number of protons in the atomic nucleus of this element,

${\displaystyle n_{1}}$ is the principal quantum number of the upper energy level, and

${\displaystyle n_{2}}$ is the principal quantum number of the lower energy level for the atomic electron transition.

This formula can be directly applied only to hydrogen-like, also called hydrogenic atoms of chemical elements, i.e. atoms with only one electron being affected by an effective nuclear charge (which is easily estimated). Examples would include He⁺, Li²⁺, Be³⁺ etc., where no other electrons exist in the atom.

But the Rydberg formula also provides correct wavelengths for distant electrons, where the effective nuclear charge can be estimated as the same as that for hydrogen, since all but one of the nuclear charges have been screened by other electrons, and the core of the atom has an effective positive charge of +1.

Finally, with certain modifications (replacement of Z by Z − 1, and use of the integers 1 and 2 for the ns to give a numerical value of ​³⁄₄ for the difference of their inverse squares), the Rydberg formula provides correct values in the special case of K-alpha lines, since the transition in question is the K-alpha transition of the electron from the 1s orbital to the 2p orbital. This is analogous to the Lyman-alpha line transition for hydrogen, and has the same frequency factor. Because the 2p electron is not screened by any other electrons in the atom from the nucleus, the nuclear charge is diminished only by the single remaining 1s electron, causing the system to be effectively a hydrogenic atom, but with a diminished nuclear charge Z − 1. Its frequency is thus the Lyman-alpha hydrogen frequency, increased by a factor of (Z − 1)². This formula of f = c/λ = (Lyman-alpha frequency)⋅(Z − 1)² is historically known as Moseley's law (having added a factor c to convert wavelength to frequency), and can be used to predict wavelengths of the K_α (K-alpha) X-ray spectral emission lines of chemical elements from aluminum to gold. See the biography of Henry Moseley for the historical importance of this law, which was derived empirically at about the same time it was explained by the Bohr model of the atom.

For other spectral transitions in multi-electron atoms, the Rydberg formula generally provides incorrect results, since the magnitude of the screening of inner electrons for outer-electron transitions is variable and not possible to compensate for in the simple manner above. The correction to the Rydberg formula for these atoms is known as the quantum defect.

See also

• Balmer series
• Hydrogen line
• Rydberg–Ritz combination principle

References

1. See:
   • Rydberg, J.R. (1889). "Researches sur la constitution des spectres d'émission des éléments chimiques" [Investigations of the composition of the emission spectra of chemical elements]. Kongliga Svenska Vetenskaps-Akademiens Handlingar [Proceedings of the Royal Swedish Academy of Science]. 2nd series (in French). 23 (11): 1–177.
   • English summary: Rydberg, J.R. (1890). "On the structure of the line-spectra of the chemical elements". Philosophical Magazine. 5th series. 29: 331–337.
2. Bohr, N. (1985). "Rydberg's discovery of the spectral laws". In Kalckar, J. (ed.). Collected works. 10. Amsterdam: North-Holland Publ. Cy. pp. 373–379.
3. Ritz, W. (1908). "Magnetische Atomfelder und Serienspektren" [The magnetic fields of atoms and spectral series]. Annalen der Physik (in German). 330 (4): 660–696. Bibcode:1908AnP...330..660R. doi:10.1002/andp.19083300403.

• Sutton, Mike (July 2004). "Getting the numbers right: The lonely struggle of the 19th century physicist/chemist Johannes Rydberg". Chemistry World. 1 (7): 38–41. ISSN 1473-7604.
• Martinson, I.; Curtis, L.J. (2005). "Janne Rydberg – his life and work". Nuclear Instruments and Methods in Physics Research Section B. 235 (1–4): 17–22. Bibcode:2005NIMPB.235...17M. CiteSeerX 10.1.1.602.6210. doi:10.1016/j.nimb.2005.03.137.