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NIST Atomic Spectra Database Lines Data

H I: 5 Lines of Data Found
Z = 1, H isoelectronic sequence 

Example of how to reference these results:
Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2021). NIST Atomic Spectra Database (ver. 5.9), [Online]. Available: https://physics.nist.gov/asd [2022, January 19]. National Institute of Standards and Technology, Gaithersburg, MD. DOI: https://doi.org/10.18434/T4W30F
BibTex Citation (new window)
 
Wavelength range: 656.2451 - 656.2882 nm
Wavelength in: vacuum
Highest relative intensity: 500000

Primary data sources
Query NIST Bibliographic Databases for
H I (new window)
Energy Levels:  Kramida 2010     Most of the given level values are essentially experimental ones. More accurate theoretical data on fine-structure energy levels and transitions between them can be obtained in the NIST Database of Energy Levels of Hydrogen and Deuterium. The levels designated only by a principal quantum number n in the configuration column represent centers of groups of all fine-structure levels having the given n. Their values were derived from line series observed in emission from solar corona and are relevant only for this type of observations. Uncertainties of the level values vary between 3 and 23 in the units of the last given decimal place. The level values in square brackets were obtained by interpolation or extrapolation of experimental fine-structure intervals or by fitting the Ritz-type formulas along series of levels. The level values in parentheses were derived from the theoretical values in the NIST Database of Energy Levels of Hydrogen and Deuterium by adding to them calculated off-diagonal magnetic-dipole hyperfine shifts. H I Energy Levels
Lines:  Kramida 2010     The lines corresponding to transitions associated with the levels designated only by the principal quantum numbers (e.g., 2-3 or 1s-2) correspond to observations in which the fine structure of transitions is completely unresolved. Their observed and calculated (Ritz) wavelengths, given here, are pertinent to observations of the solar corona. The observed intensity values of these lines, given in arbitrary units, are pertinent to the same type of observations. Intensity values given in parentheses are extrapolated values. Relative intensities of lines in laboratory light sources differ from those in the solar corona by several orders of magnitude and strongly depend on experimental conditions. Wavelengths of centers of gravity and various blended groups of fine-structure components of the Balmer series lines, derived assuming Boltzmann populations in an optically thin medium, are given without level classifications. Their identities and uncertainties are explained in the "Line Ref." column. H I Line Wavelengths and Classification
Transition Probabilities:  Wiese and Fuhr 2009  H I Transition Probabilities


 Observed 
 Wavelength 
 Vac (nm) 
 Unc. 
 (nm) 
 Ritz 
 Wavelength 
 Vac (nm) 
 Unc. 
 (nm) 
 Transition 
 Wavenumber 
 (cm-1
 Rel. 
 Int. 
(?)
 Aki
 (s-1
 Acc.   Ei 
 (cm-1
   Ek 
 (cm-1
 Lower Level 
 Conf., Term, J 
 Upper Level 
 Conf., Term, J 
 Type   TP
Ref.
 Line
Ref.
                                       
656.4522552  0.0000024  656.4522556  0.0000009  15 233.40033      5.3877e+07    AAA 82 258.9191133     97 492.319433   2p   2P°   1/2   3d   2  3/2  T8637 L2752
656.4537684  0.0000004  656.4537685  0.0000003  15 233.365214     2.2448e+07    AAA 82 258.9543992821  97 492.319611   2s   2  1/2   3p   2P°   3/2  T8637 L6891c38
656.4584404  0.0000004  656.4584403  0.0000003  15 233.256799     2.2449e+07    AAA 82 258.9543992821  97 492.211200   2s   2  1/2   3p   2P°   1/2  T8637 L6891c38
656.460      0.003      656.4632     0.0007     15 233.21       500000  4.4101e+07    AAA 82 259.158         97 492.304      2         3        T8637 L7400c29
656.466464   0.000006   656.4664660  0.0000003  15 233.07061      6.4651e+07    AAA 82 259.2850014     97 492.355566   2p   2P°   3/2   3d   2  5/2  T8637 L2752

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