Calculating the Balmer Alpha Line: Atomic Hydrogen

[neilparker62]

Introduction
Most readers acquainted with the hydrogen spectrum will be familiar with the set of lines in the visible spectrum representing transitions of electrons from energy levels 3,4,5 and 6 (H alpha, beta, gamma, and delta respectively)  of atomic hydrogen to energy level 2 – the Balmer series lines. The picture below shows 3 of these lines (amongst others) in a diffraction grating image of the solar chromosphere during a total eclipse of the sun. For a very brief moment, the normal dark Fraunhofer lines of the solar absorption spectrum become an emission spectrum. The diffraction grating then shows separated images of the eclipse at various prominent wavelengths (indicated in the diagram) within the chromospheric emission spectrum. See also: The Spectrum of the...

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[eljose79]

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Hello there,

Thank you for bringing up this interesting topic about the hydrogen spectrum and its appearance during a total eclipse of the sun. I find this phenomenon to be quite fascinating and worth further investigation.

The Balmer series lines, as you mentioned, are a set of spectral lines that are observed when electrons in hydrogen atoms transition from higher energy levels to the second energy level. These transitions result in the emission of photons at specific wavelengths, which can be seen as lines in the spectrum. These lines are named after Johann Balmer, who first discovered this series in 1885.

During a total eclipse of the sun, the normal dark lines in the solar absorption spectrum become an emission spectrum due to the presence of the solar chromosphere. This is a thin layer of the sun's atmosphere that is only visible during a total eclipse. The chromosphere is much hotter than the layers above it, which causes it to emit light at specific wavelengths, including those of the Balmer series lines.

The diffraction grating image of the solar chromosphere during a total eclipse is a valuable tool for studying the hydrogen spectrum. By analyzing the separated images at different wavelengths, we can determine the intensity and distribution of the Balmer series lines. This information can provide insights into the composition and temperature of the chromosphere.

In addition to the Balmer series lines, there are also other spectral lines that can be observed in the solar chromosphere, such as the Lyman series lines, which correspond to transitions to the first energy level of hydrogen. These lines can also be seen in the diffraction grating image, but they are typically fainter than the Balmer series lines.

Overall, the study of the hydrogen spectrum during a total eclipse is an exciting area of research that can help us better understand the properties of the sun's atmosphere. Thank you for sharing this topic, and I look forward to reading more about it in the future.