The spectrum of WR 42e shows many characteristics of an OIf * star, such as hydrogen Balmer series absorption lines and emission lines of ionised nitrogen and helium.
12.
The visual spectrum of Vega is dominated by absorption lines of hydrogen; specifically by the hydrogen Balmer series with the electron at the n = 2 principal quantum number.
13.
The solution of this equation for atoms led to the explanation of the Balmer series for atomic spectra and consequently formed a basis for all of atomic physics and chemistry.
14.
Due to the prevalence of hydrogen in interstellar gas, and its relatively low energy of ionization, many emission nebulae appear red due to the strong emissions of the Balmer series.
15.
The spectral classification of stars, which is primarily a determination of surface temperature, is based on the relative strength of spectral lines, and the Balmer series in particular is very important.
16.
Emission spectra from W . M . Keck Observatory, obtained by Palomar Transient Factory indicate that this is a type II supernova with a relatively blue continuum with P Cygni profiles in the Balmer series.
17.
N III and N IV emission lines lines are stronger than N V, and He I lines are stronger than He II, The Balmer series hydrogen lines and some other lines have P Cygni profiles.
18.
The star appears, based on its spectrum in the Balmer series, to be a blue supergiant, although in reality it is an old low-mass star on the post-AGP phase of its life.
19.
The H ? emission is often unusually strong compared to other lines of the Balmer series in a normal M star, but this is due to the weakness of the TiO band that would otherwise dilute the H ? emission.
20.
The Balmer series is characterized by the electron transitioning from " n " e " 3 to " n " = 2, where " n " refers to the radial quantum number or principal quantum number of the electron.
