Pickering series

The Pickering series (also known as the Pickering–Fowler series) consists of three lines of singly ionised helium found, usually in absorption, in the spectra of hot stars like Wolf–Rayet stars. The name comes from Edward Charles Pickering^[1] and Alfred Fowler.^[2] The lines are produced by transitions from a higher energy level of an electron to a level with principal quantum number n = 4. The lines have wavelengths:

• 10124 Å (n = 5 to n = 4) (infrared)
• 6560 Å (n = 6 to n = 4)  
• 5412 Å (n = 7 to n = 4)  
• 4859 Å (n = 8 to n = 4)  
• 4541 Å (n = 9 to n = 4)  
• 4339 Å (n = 10 to n = 4)  
• 3645.56 Å (n = ∞ to n = 4, theoretical limit, ultraviolet)

The transitions from the even-n states overlap with hydrogen lines and are therefore masked in typical absorption stellar spectra. However, they are seen in emission in the spectra of Wolf-Rayet stars, as these stars have little or no hydrogen.

In 1896, Pickering published observations of previously unknown lines in the spectra of the star Zeta Puppis.^[3] Pickering attributed the observation to a new form of hydrogen with half-integer transition levels.^[4][5] Fowler managed to produce similar lines from a hydrogen–helium mixture in 1912, and supported Pickering's conclusion as to their origin.^[6] Niels Bohr, however, included an analysis of the series in his 'trilogy'^[7][8] on atomic structure^[9] and concluded that Pickering and Fowler were wrong and that the spectral lines arise instead from singly ionised helium, He⁺.^[10] Fowler was initially skeptical^[11] but was ultimately convinced^[12] that Bohr was correct,^[7] and by 1915 "spectroscopists had transferred [the Pickering series] definitively [from hydrogen] to helium."^[1][13] Bohr's theoretical work on the Pickering series had demonstrated the need for "a re-examination of problems that seemed already to have been solved within classical theories" and provided important confirmation for his atomic theory.^[1]

Wavelength formula

Main article: Rydberg formula

The energy differences between levels in the Bohr model, and hence the wavelengths of emitted or absorbed photons, is given by the Rydberg formula:^[14] $${\displaystyle {\frac {1}{\lambda }}=Z^{2}R_{M}\left({\frac {1}{{n_{1}}^{2}}}-{\frac {1}{{n_{2}}^{2}}}\right)}$$ where

• ${\displaystyle Z}$ is the atomic number,
• ${\displaystyle n_{1}}$ is the principal quantum number of the lower energy level,
• ${\displaystyle n_{2}}$ is the principal quantum number of the upper energy level, and
• ${\displaystyle R_{M}}$ is the Rydberg constant for a nucleus of mass ${\displaystyle M}$. It follows ${\displaystyle R_{M}={\frac {\mu }{m_{e}}}R_{\infty }}$ with ${\displaystyle \mu }$ the reduced mass of the nucleus and ${\displaystyle R_{\infty }={\frac {m_{e}{q_{e}}^{4}}{64\pi ^{3}{\varepsilon _{0}}^{2}\hbar ^{3}c}}}$ is Rydberg constant.

For helium, ${\displaystyle Z=2}$, the Pickering-Fowler series is for ${\displaystyle n_{1}=4}$ and the reduced mass for ${\displaystyle {}_{2}^{4}{\text{He}}^{+}}$ is ${\displaystyle \mu ={\frac {1}{{\frac {1}{m_{e}}}+{\frac {1}{2m_{p}+2m_{n}}}}}}$ thus ${\displaystyle {\frac {\mu }{m_{e}}}={\frac {1}{1+{\frac {m_{e}}{2m_{p}+2m_{n}}}}}\approx 0.99986396}$, which is usually approximated as ${\displaystyle 1}$ (in fact, although this number changes for each isotope of helium, it is approximately constant). A more accurate description may be used with the Bohr–Sommerfeld model of the atom.

The theoretical limit for the wavelength in the Pickering-Fowler is given by: ${\displaystyle \lambda _{\infty }^{\text{PF}}={\frac {4}{R_{\infty }}}}$, which is approximatedly 364.556 nm, which is the same limit as in the Balmer series (hydrogen spectral series for ${\displaystyle n_{2}=2}$). Notice how the transitions in the Pickering-Fowler series for n=6,8,10 (6560Å ,4859Å and 4339Å respectively), are nearly identical to the transitions in the Balmer series for n=3,4,5 (6563Å ,4861Å and 4340Å respectively). The fact that the Pickering-Fowler series has entries inbetween those values, led scientist to believe it was due to hydrogen with half transitions ("half-hydrogen"). However, Niels Bohr showed, using his model, it was due to the singly ionised helium ${\displaystyle {}_{2}{\text{He}}^{+}}$, a hydrogen-like atom. This also shows the predictability of Bohr model.

References

1. Robotti, Nadia (1983). "The Spectrum of ζ Puppis and the Historical Evolution of Empirical Data". Historical Studies in the Physical Sciences. 14 (1): 123–145. doi:10.2307/27757527. JSTOR 27757527.
2. Lakatos, Imre (1980). "Bohr: A Research Programme Progressing on Inconsistent Foundations". In Worrall, John; Currie, Gregory (eds.). The Methodology of Scientific Research Programmes. Cambridge University Press. pp. 55–68. ISBN 9780521280310.
3. Pickering, E. C. (1896). "Stars having peculiar spectra. New variable stars in Crux and Cygnus". Harvard College Observatory Circular. 12: 1–2. Bibcode:1896HarCi..12....1P. Also published as: Pickering, E. C.; Fleming, W. P. (1896). "Stars having peculiar spectra. New variable stars in Crux and Cygnus". Astrophysical Journal. 4: 369–370. Bibcode:1896ApJ.....4..369P. doi:10.1086/140291.
4. Pickering, E. C. (1897). "Stars having peculiar spectra. New variable Stars in Crux and Cygnus". Astronomische Nachrichten. 142 (6): 87–90. Bibcode:1896AN....142...87P. doi:10.1002/asna.18971420605.
5. Pickering, E. C. (1897). "The spectrum of zeta Puppis". Astrophysical Journal. 5: 92–94. Bibcode:1897ApJ.....5...92P. doi:10.1086/140312.
6. Fowler, A. (1912). "Observations of the Principal and other Series of Lines in the Spectrum of Hydrogen". Monthly Notices of the Royal Astronomical Society. 73 (2): 62–63. Bibcode:1912MNRAS..73...62F. doi:10.1093/mnras/73.2.62.
7. Hoyer, Ulrich (1981). "Constitution of Atoms and Molecules". In Hoyer, Ulrich (ed.). Niels Bohr – Collected Works: Volume 2 – Work on Atomic Physics (1912–1917). Amsterdam: North Holland Publishing Company. pp. 103–316 (esp. pp. 116–122). ISBN 978-0720418002.
8. Kennedy, P. J. (1985). "A Short Biography". In French, A. P.; Kennedy, P. J. (eds.). Niels Bohr: A Centenary Volume. Harvard University Press. pp. 3–15. ISBN 978-0-674-62415-3.
9. Bohr, N. (1913). "On the constitution of atoms and molecules, part I" (PDF). Philosophical Magazine. 26 (151): 1–25. Bibcode:1913PMag...26....1B. doi:10.1080/14786441308634955.
   Bohr, N. (1913). "On the constitution of atoms and molecules, part II: Systems Containing Only a Single Nucleus" (PDF). Philosophical Magazine. 26 (153): 476–502. Bibcode:1913PMag...26..476B. doi:10.1080/14786441308634993.
   Bohr, N. (1913). "On the constitution of atoms and molecules, part III: Systems containing several nuclei". Philosophical Magazine. 26 (155): 857–875. Bibcode:1913PMag...26..857B. doi:10.1080/14786441308635031.
10. Bohr, N. (1913). "The Spectra of Helium and Hydrogen". Nature. 92 (2295): 231–232. Bibcode:1913Natur..92..231B. doi:10.1038/092231d0. S2CID 11988018.
11. Fowler, A. (1913). "The Spectra of Helium and Hydrogen". Nature. 92 (2291): 95–96. Bibcode:1913Natur..92...95F. doi:10.1038/092095b0. S2CID 3972599.
12. Fowler, A. (1913). "Reply to: The Spectra of Helium and Hydrogen". Nature. 92 (2295): 232–233. Bibcode:1913Natur..92..232F. doi:10.1038/092232a0. S2CID 3981817.
13. Bohr, N. (1915). "The Spectra of Hydrogen and Helium". Nature. 95 (6–7): 6–7. Bibcode:1915Natur..95....6B. doi:10.1038/095006a0. S2CID 3947572.
14. Bohr, Niels (1985), "Rydberg's discovery of the spectral laws", in Kalckar, J. (ed.), N. Bohr: Collected Works, vol. 10, Amsterdam: North-Holland Publ., pp. 373–9

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