Parts of the Balmer series can be seen in the solar spectrum.

These were later identified as lines from the Hydrogen Balmer series.

The difference between energy levels recovers the Balmer series.

The solution for the hydrogen atom describes standing waves of energy exactly given by the Balmer series.

The spectral lines of hydrogen had been analyzed and found to have a mathematical relationship in the Balmer series.

Balmer lines and Balmer series are named after him.

The Bohr model, introduced in 1913, was an attempt to provide a theoretical basis for the Balmer series.

Rydberg managed to find a formula to match the known Balmer series emission lines, and also predicted those not yet discovered.

Balmer series in hydrogen (Bohr's old quantum theory).

The Balmer series of hydrogen lines grows stronger through the B class, then peak at type A2.

The Bohr assumptions recover the observed Balmer series.

The Balmer series identifies those frequencies of light that can be emitted from an excited hydrogen atom:

The apparent Lyman-α cross sections for all three targets contained significant cascade contributions from the H Balmer series.

Many spectral lines of atomic hydrogen also have designations within their respective series, such as the Lyman series or Balmer series.

In 1885, Johann Balmer had come up with his Balmer series to describe the visible spectral lines of a hydrogen atoms:

The Balmer series is calculated using the Balmer formula, an empirical equation discovered by Johann Balmer in 1885.

Emission lines of hydrogen (mainly of the Lyman series and Balmer series), helium, carbon, magnesium, iron and oxygen are the brightest lines.

In the outer region of the ring, part of the reddish hue is caused by hydrogen emission at 656.3 nm, forming part of the Balmer series of lines.

Choice of modern physics experiments including speed of light, measurement of e/m, Balmer series of hydrogen, photoelectric effect, the Millikan oil drop and Frank-Hertz experiments.

His Ph.D. degree was awarded in 1941 for a dissertation on "The Formation of the Balmer Series of Hydrogen in Stellar Atmospheres."

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.

At the limit of the Balmer series a change happens where at shorter wavelengths more bound-bound Balmer series transitions cause more opacity.

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 are very important.

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.

The Balmer series or Balmer lines in atomic physics, is the designation of one of a set of six named series describing the spectral line emissions of the hydrogen atom.