“hydrogen spectrum”的概念、定义、翻译、参考文献-科学参考

hydrogen spectrum

Physics

The atomic spectrum of hydrogen is characterized by lines corresponding to radiation quanta of sharply defined energy. A graph of the frequencies at which these lines occur against the ordinal number that characterizes their position in the series of lines produces a smooth curve, indicating that they obey a formal law. In 1885 Johann Jakob Balmer (1825–98) discovered the law, having the form

$1 / λ = R (1 / n_{1}^{2} - 1 / n_{2}^{2})$

This law gives the so-called Balmer series of lines in the visible spectrum, in which n₁=2 and n₂=3,4,5,…, λ‎ is the wavelength associated with the lines, and R is the Rydberg constant.

In the Lyman series, discovered by Theodore Lyman (1874–1954), n₁=1 and the lines fall in the ultraviolet. The Lyman series is the strongest feature of the solar spectrum as observed by rockets and satellites above the earth’s atmosphere. In the Paschen series, discovered by Friedrich Paschen (1865–1947), n₁=3 and the lines occur in the far infrared. The Brackett series (n₁=4), Pfund series (n₁=5), and Humphreys series (n₁=6) also occur. See also Fock degeneracy.

http://web.lemoyne.edu/~giunta/balmer.html A translation of Balmer’s 1885 paper on the spectral lines of hydrogen in Annalen der Physik und Chemie

Astronomy

A distinctive pattern of spectral lines, either emission or absorption, produced by hydrogen, the simplest of all the atoms. The series of lines in the spectrum are labelled according to the lowest energy level involved in the transitions that give rise to the lines. If an electron jumps to or from the ground state (n = 1), it produces a line in the Lyman series; n = 2 corresponds to the Balmer series; n = 3 to the Paschen series; n = 4 to the Brackett series; n = 5 to the Pfund series; and n = 6 to the Humphreys series. The Balmer series lines fall in the visible part of the spectrum, the Paschen, Brackett, Pfund, and Humphreys series are in the infrared, and the Lyman series is in the ultraviolet.

Chemistry

The atomic spectrum of hydrogen is characterized by lines corresponding to radiation quanta of sharply defined energy. A graph of the frequencies at which these lines occur against the ordinal number that characterizes their position in the series of lines, produces a smooth curve indicating that they obey a formal law. In 1885 Johann Jakob Balmer (1825–98) discovered the law having the form:
$1 / λ = R (1 / n_{1}^{2} - 1 / n_{2}^{2})$
This law gives the so-called Balmer series of lines in the visible spectrum in which n₁ = 2 and n₂ = 3,4,5…, λ‎ is the wavelength associated with the lines, and R is the Rydberg constant.
In the Lyman series, discovered by Theodore Lyman (1874–1954), n₁ = 1 and the lines fall in the ultraviolet. The Lyman series is the strongest feature of the solar spectrum as observed by rockets and satellites above the earth’s atmosphere. In the Paschen series, discovered by Friedrich Paschen (1865–1947), n₁ = 3 and the lines occur in the far infrared. The Brackett series (n₁ = 4), Pfund series (n₁ = 5), and Humphreys series (n₁ = 6) also occur in the far infrared. The occurrence of the Balmer series and other series of the hydrogen atom spectrum can be derived quantitatively using quantum mechanics. A full understanding of the hydrogen atom spectrum requires the concept of Fock degeneracy.
http://web.lemoyne.edu/~giunta/balmer.html Balmer’s paper

单词	hydrogen spectrum
释义	hydrogen spectrum Physics The atomic spectrum of hydrogen is characterized by lines corresponding to radiation quanta of sharply defined energy. A graph of the frequencies at which these lines occur against the ordinal number that characterizes their position in the series of lines produces a smooth curve, indicating that they obey a formal law. In 1885 Johann Jakob Balmer (1825–98) discovered the law, having the form $1 / λ = R (1 / n_{1}^{2} - 1 / n_{2}^{2})$ This law gives the so-called Balmer series of lines in the visible spectrum, in which n₁=2 and n₂=3,4,5,…, λ‎ is the wavelength associated with the lines, and R is the Rydberg constant. In the Lyman series, discovered by Theodore Lyman (1874–1954), n₁=1 and the lines fall in the ultraviolet. The Lyman series is the strongest feature of the solar spectrum as observed by rockets and satellites above the earth’s atmosphere. In the Paschen series, discovered by Friedrich Paschen (1865–1947), n₁=3 and the lines occur in the far infrared. The Brackett series (n₁=4), Pfund series (n₁=5), and Humphreys series (n₁=6) also occur. See also Fock degeneracy. http://web.lemoyne.edu/~giunta/balmer.html A translation of Balmer’s 1885 paper on the spectral lines of hydrogen in Annalen der Physik und Chemie Astronomy A distinctive pattern of spectral lines, either emission or absorption, produced by hydrogen, the simplest of all the atoms. The series of lines in the spectrum are labelled according to the lowest energy level involved in the transitions that give rise to the lines. If an electron jumps to or from the ground state (n = 1), it produces a line in the Lyman series; n = 2 corresponds to the Balmer series; n = 3 to the Paschen series; n = 4 to the Brackett series; n = 5 to the Pfund series; and n = 6 to the Humphreys series. The Balmer series lines fall in the visible part of the spectrum, the Paschen, Brackett, Pfund, and Humphreys series are in the infrared, and the Lyman series is in the ultraviolet. Chemistry The atomic spectrum of hydrogen is characterized by lines corresponding to radiation quanta of sharply defined energy. A graph of the frequencies at which these lines occur against the ordinal number that characterizes their position in the series of lines, produces a smooth curve indicating that they obey a formal law. In 1885 Johann Jakob Balmer (1825–98) discovered the law having the form: $1 / λ = R (1 / n_{1}^{2} - 1 / n_{2}^{2})$ This law gives the so-called Balmer series of lines in the visible spectrum in which n₁ = 2 and n₂ = 3,4,5…, λ‎ is the wavelength associated with the lines, and R is the Rydberg constant. In the Lyman series, discovered by Theodore Lyman (1874–1954), n₁ = 1 and the lines fall in the ultraviolet. The Lyman series is the strongest feature of the solar spectrum as observed by rockets and satellites above the earth’s atmosphere. In the Paschen series, discovered by Friedrich Paschen (1865–1947), n₁ = 3 and the lines occur in the far infrared. The Brackett series (n₁ = 4), Pfund series (n₁ = 5), and Humphreys series (n₁ = 6) also occur in the far infrared. The occurrence of the Balmer series and other series of the hydrogen atom spectrum can be derived quantitatively using quantum mechanics. A full understanding of the hydrogen atom spectrum requires the concept of Fock degeneracy. http://web.lemoyne.edu/~giunta/balmer.html Balmer’s paper
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