The Balmer jump, Balmer discontinuity, or Balmer break is the difference of intensity of the stellar continuum spectrum on either side of the limit of the Balmer series of hydrogen, at approximately 364.5 nm.

Jan 30, 2023 · Balmer Jump is caused by electrons being completely ionized directly from the second energy level of a hydrogen atom (bound-free absorption), which creates a continuum absorption at wavelengths shorter than 364.5 nm.

May 28, 2024 · The Balmer Jump is a fundamental concept in astrophysics, providing essential clues about the physical properties of stars and their evolutionary stages. Its study enhances our understanding of stellar atmospheres and contributes to the broader field of cosmic exploration.

The Balmer series, or Balmer lines in atomic physics, is one of a set of six named series describing the spectral line emissions of the hydrogen atom. The Balmer series is calculated using the Balmer formula, an empirical equation discovered by Johann Balmer in 1885.

The Balmer jump (or Balmer discontinuity, Balmer edge, or Balmer break) is a spectral feature consisting of a steep downward slope within an object's SED (sloping downward as you look at shorter and shorter wavelengths) at the Balmer limit, the "infinity end" of the Balmer series spectral lines, which is 364.6 nm.

Mar 20, 2024 · In astronomy, the Balmer Jump is a valuable tool for studying the properties of stars and galaxies. By analyzing the intensity of radiation at the Balmer limit, astronomers can determine the temperature and density of the gas surrounding celestial objects.

balmer jump The 3647 Å Balmer Jump in the spectra of the hot star alpha Lyra (Vega), observed by Barbier and Chalonge (1939). Sir William Huggins was the first to observe the Balmer jump at the turn of the century in the stellar spectra of Vega and similar stars.

Nov 22, 2024 · This explanation is supported by the presence of a Balmer break (sometimes also called a Balmer jump) in the spectra of some LRDs. A Balmer break refers to a significant dip in a spectrum for wavelengths shorter than the Balmer limit – or, the maximum wavelength of light which can ionise a hydrogen atom with an electron in the second energy ...

The Balmer jump, Balmer discontinuity, or Balmer break is the difference of intensity of the stellar continuum spectrum on either side of the limit of the Balmer series of hydrogen, at approximately 364.5 nm.

The Balmer jump is produced by a rapid drop of the total Balmer cross-section, yet this variation is smooth and continuous when both bound-bound and bound-free processes are taken into account, and its shape and location is dependent on the broadening mechanisms.