From Johann Jakob Balmer (1825-1898), Swiss mathematician and physicist, who explained the visible spectral lines of the hydrogen spectrum in 1885.
Fr.: continuum de Balmer
A continuous range of wavelengths in the Balmer spectrum of
hydrogen corresponding to transitions between the energy levels
Fr.: décrément de Balmer
The intensity ratio among the couple of relatively adjacent → Balmer lines, for example Hα/Hβ and Hβ/Hγ, which have well-known theoretical values. They are used to determine the → interstellar extinction.
Fr.: discontinuité de Balmer
An abrupt decrease in the intensity of the continuum at the limit of the → Balmer series of hydrogen (at about 3650 Å), caused by the energy absorbed when electrons originally in the second → energy level are ionized. Same as → Balmer jump.
→ Balmer; → discontinuity.
Fr.: formule de Balmer
A special solution of the mathematical formula which represents
the wavelengths of the various spectral series of hydrogen in which the
lower energy level is n =
Fr.: saut de Balmer
Same as → Balmer discontinuity.
Fr.: limite de Balmer
The wavelength in the blue end of the → Balmer series, at 3646 Å, near which the separation between successive lines decreases and approaches a → continuum.
Fr.: raies de Balmer
The → spectral lines making up the → Balmer series.
seri-ye Bâlmer (#)
Fr.: série de Balmer
A series of hydrogen → spectral lines
(Hα, Hβ, Hγ, and others) that lies in the visible
portion of the spectrum and results when electrons from upper
→ energy levels (n > 2) undergo
→ transition to n =