Balmer series
The Balmer series is the name given to a series of spectral emission lines of the hydrogen atom that result from electron transitions from higher levels down to the energy level with principal quantum number 2.
Balmer series (J. Balmer; 1885)
An equation which describes the emission spectrum of hydrogen when an electron is jumping to the second orbital. Four of the lines are in the visible spectrum; the remainder are in the ultraviolet.
BALMER SERIES - Hydrogen series of emission that results when an electron drops into the second orbital. Four of the lines are in the visible spectrum, and the remainder is in the ultraviolet.
Balmer Series
(a) A series of lines in the spectrum of radiation emitted by excited hydrogen atoms. The lines correspond to the atomic electrons falling into the second lowest energy level, emitting energy as radiation.
Balmer series: Spectral lines in the visible and near-ultraviolet spectrum of hydrogen produced by transitions whose lowest orbit is the second.
Balmer Series - A series of absorption or emission lines of hydrogen seen in the visible part of the spectrum
Barred Spiral Galaxy - A spiral galaxy in which the nucleus is crossed by a bar. The spiral arms start at the ends of the bar ...
Balmer series . A series of 4 visible colors emitted by glowing hydrogen, appearing as a series of 4 "lines" in the spectrogram of hydrogen light (additional lines can be observed by instruments, beyond the range of the human eye).
The Balmer series of visible lines for atomic hydrogen are caused by transitions from the n = 2 orbit to and from higher orbits. This is shown schematically in the diagram below for the Bohr model of the atom.
The next series of lines, the Balmer series, involves transitions down to (or up from) level 2, the first excited state. All the Balmer series lines lie in or close to the visible portion of the electromagnetic spectrum.
When people first started taking spectra of stars, they noticed that stars had very different hydrogen spectral lines strengths, and so they classified stars based on the strength of the hydrogen Balmer series lines from A (strongest) to Q (weakest).
An early classification of spectra by Angelo Secchi in the 1860s divided stars into those with prominent lines from the hydrogen Balmer series (group I, with a subtype representing many of the stars in Orion); those with spectra which, like the Sun, ...
Balmer series). The spectra of stars with still lower surface temperatures manifest different absorption line patterns.
A star of spectral type A, white in color, with a spectrum dominated by the Balmer series of hydrogen. Lines of heavy elements, such as iron, are noticeable at the cooler end of the range.
The sudden decrease in the intensity of the continuous spectrum at the limit of the Balmer series of hydrogen at 3646 Å, representing the energy absorbed when electrons originally in the second energy level are ionized.
Stellar spectra
Absorption lines from photosphere
Hydrogen Balmer series changes in strength :
weak at low temp : all in ground state (n=1)
weak at high temp : all ionized
strongest at about 10,000K (A0 stars) ...
The first line of the Balmer series of hydrogen, at 6563 angstroms.
hadron epoch - (n.) ...
 See also: Spectrum, Hydrogen, Time, Element, Energy
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