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Important atomic emission spectra
of atomic hydrogen has been divided into a number of spectral series, with wavelengths given by the Rydberg formula. These observed spectral lines are
Hydrogen_spectral_series
Hydrogen spectral series
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
Deep-red spectral line of hydrogen
nm in vacuum. It is the first spectral line in the Balmer series and is emitted when an electron falls from a hydrogen atom's third- to second-lowest
Hydrogen-alpha
Formula for spectral line wavelengths in alkali metals
wavelengths of the hydrogen spectral series. In 1890, Rydberg proposed on a formula describing the relation between the wavelengths in spectral lines of alkali
Rydberg_formula
Set of ultraviolet wavelengths emitted by hydrogen
chemistry, the Lyman series is a hydrogen spectral series of transitions and resulting ultraviolet emission lines of the hydrogen atom as an electron goes
Lyman_series
One over a whole number
optimization and in analyzing the pattern of frequencies in the hydrogen spectral series. The unit fractions are the rational numbers that can be written
Unit_fraction
Physical constants of energy and wavenumber
an empirical fitting parameter in the Rydberg formula for the hydrogen spectral series, but Niels Bohr later showed that its value could be calculated
Rydberg_constant
Spectral line of hydrogen state transition in UHF radio frequencies
The hydrogen line, 21 centimeter line, or H I line is a spectral line that is created by a change in the energy state of solitary, electrically neutral
Hydrogen_line
Distinctive narrow spectral feature of chemical species
lines). Many spectral lines of atomic hydrogen also have designations within their respective series, such as the Lyman series or Balmer series. Originally
Spectral_line
Difference of intensity of the stellar continuum spectrum
when the Balmer lines themselves are strongly in emission. Other hydrogen spectral series also show bound-free absorption and hence a continuum discontinuity
Balmer_jump
Atom of the element hydrogen
number). Bohr's predictions matched experiments measuring the hydrogen spectral series to the first order, giving more confidence to a theory that used
Hydrogen_atom
Chemical element with atomic number 1 (H)
levels of hydrogen are referred to by consecutive quantum numbers, with n = 1 {\displaystyle n=1} being the ground state. The hydrogen spectral series corresponds
Hydrogen
Material composed of antiparticles
symmetry through comparison of the atomic spectra of hydrogen and antihydrogen (see hydrogen spectral series). Most of the sought-after high-precision tests
Antimatter
American physicist
ISSN 0003-3804. Slack, Francis G. (1928-04-01). "Intensities in the Hydrogen Spectral Series". Physical Review. 31 (4). American Physical Society (APS): 527–532
Francis_G._Slack
Study involving matter and electromagnetic radiation
reproduced the spectral lines of hydrogen. These equated discrete quantum jumps of the bound electron in a hydrogen atom to the discrete hydrogen spectrum.
Spectroscopy
Description of a quantum-mechanical system
correct spectral energies of hydrogen in a paper published in 1926. Schrödinger computed the hydrogen spectral series by treating a hydrogen atom's electron
Schrödinger_equation
American physicist
hydrogen spectral series Pfund discovered the fifth series, where an electron jumps up from or drops down to the fifth fundamental level. This Series
August_Herman_Pfund
the Balmer series (hydrogen spectral series for n 2 = 2 {\displaystyle n_{2}=2} ). Notice how the transitions in the Pickering-Fowler series for n=6,8
Pickering_series
Supernova event observed on September 29, 2005
IIn supernovae, and because hydrogen emission lines were found in its spectrum (see hydrogen spectral series). These hydrogen lines, which were found on
SN_2005gj
Elementary particle with negative charge
element or molecule displays a characteristic set of spectral lines, such as the hydrogen spectral series. When detected, spectroscopic measurements of the
Electron
Topics referred to by the same term
levels in the presence of a strong magnetic field Paschen series, a Hydrogen spectral series in the infrared band Paschen's law, an equation that gives
Paschen
Quasiparticle which is a bound state of an electron and an electron hole
edge of the band, forming a series of spectral absorption lines that are in principle similar to hydrogen spectral series. In a bulk semiconductor, a
Exciton
Classification of stars based on spectral properties
dwarf types are as follows: DA – a hydrogen-rich atmosphere or outer layer, indicated by strong Balmer hydrogen spectral lines. DB – a helium-rich atmosphere
Stellar_classification
Stellar classification distinguished by bright blue luminosity
B-type main-sequence star is a main-sequence (core hydrogen-burning) star of spectral type B. The spectral luminosity class is given as V. These stars have
B-type_main-sequence_star
Spectral emission line produced by the transition of electrons between two energy levels
neutral hydrogen regions. For hydrogen, this effect occurs in H II regions and can be thought of as a rarer example of the hydrogen spectral series, only
Radio_Recombination_Lines
Wave equations respecting special and general relativity
equations found by Schrödinger could predict the fine structure in the Hydrogen spectral series. The mysterious underlying property was spin. The first two-dimensional
Relativistic_wave_equations
Stellar classification
subdwarf stars, that is stars of luminosity class VI, of spectral class G. These stars are fusing hydrogen in their cores like normal main-sequence stars, but
G-type_main-sequence_star
Brightenings in the Sun's photosphere
photosphere. They are only observed in the wings of the Hα, Hβ, and Hγ hydrogen spectral lines and take place in emerging flux regions where emerging magnetic
Ellerman_bomb
Heterogeneous class of stars with unusual spectra
their spectral classification. Classic (or population I) Wolf–Rayet stars are evolved, massive stars that have completely lost their outer hydrogen and
Wolf–Rayet_star
Total eclipse
University of Colorado analyzed the spectrum of the Balmer series in the hydrogen spectral series. In addition, French astronomer Bernard Ferdinand Lyot,
Solar eclipse of February 25, 1952
Solar_eclipse_of_February_25,_1952
Stellar classification
F-type main-sequence star is a main-sequence, core-hydrogen-fusing star of spectral type F. The spectral luminosity class is V. They have from around 1.1
F-type_main-sequence_star
Swiss mathematician (1825–1898)
spectral series. His major contribution (made at the age of sixty, in 1885) was an empirical formula for the visible spectral lines of the hydrogen atom
Johann_Jakob_Balmer
Spectral line of hydrogen in the Lyman series
denoted by Ly-α or Lyα, is a spectral line of hydrogen (or, more generally, of any one-electron atom) in the Lyman series. A photon is emitted when the
Lyman-alpha
Particle storage ring at CERN, Switzerland
symmetry through comparison of the atomic spectra of hydrogen and antihydrogen (see hydrogen spectral series). The ALPHA collaboration consists of some former
Antiproton_Decelerator
Chemical compound
Triatomic hydrogen or H3 is an unstable triatomic molecule containing only hydrogen. Since this molecule contains only three atoms of hydrogen it is the
Triatomic_hydrogen
Dim, low mass stars on the main sequence
into spectral types L2 or L3. At the same time, many objects cooler than about M6 or M7 are brown dwarfs, insufficiently massive to sustain hydrogen-1 fusion
Red_dwarf
Blazar in the constellation Libra
highly eccentric orbit of a secondary black hole. By measuring hydrogen spectral series and iron emission lines, scientists were able to identify a dark
PKS_1510−089
Stellar classification
dwarf" or "orange dwarf") is a main-sequence (core hydrogen-burning) star of spectral type K. The spectral luminosity class is V. These stars are intermediate
K-type_main-sequence_star
Atomic model introduced by Niels Bohr in 1913
modern view that the spectral lines result from energy differences. In 1910, Arthur Erich Haas proposed a model of the hydrogen atom with an electron
Bohr_model
Type of star that is massive and luminous
range from about 3,400 K to over 20,000 K. Hertzsprung–Russell diagram Spectral type O B A F G K M L T Brown dwarfs White dwarfs Red dwarfs Subdwarfs Main
Supergiant
Possible type of luminous blue compact galaxy
extinction-corrected luminosity > 3×1040 ergs/s of the hydrogen beta emission line; (see hydrogen spectral series) b) a high equivalent width greater than 5 nm;
Pea_galaxy
Brown dwarf or exoplanet with atmospheric methane
than the hydrogen burning minimum mass (0.075 M☉ or 78.5 MJ). There are currently 920 objects in the UltracoolSheet with an infrared spectral type of T
T_dwarf
Methods of visualizing information by translating to colors
(metameric failure): Different spectral sensitivities of the human eye and of an image capture device (e.g. a camera). Different spectral emissions / reflections
False_color
Concept in computer programming
Microsoft CEO, Steve Ballmer, and is likely a play on Balmer series of hydrogen spectral lines named for the scientist Johann Balmer. A San Francisco
Ballmer_Peak
Series of lines in atomic spectra
The diffuse series is a series of spectral lines in the atomic emission spectrum caused when electrons jump between the lowest p orbital and d orbitals
Diffuse_series
Stellar classification
main-sequence (core hydrogen burning) star of spectral type A. The spectral luminosity class is V. These stars have spectra defined by strong hydrogen Balmer absorption
A-type_main-sequence_star
Hot, luminous star with a spectral type of A9 or earlier
Hertzsprung–Russell diagram Spectral type O B A F G K M L T Brown dwarfs White dwarfs Red dwarfs Subdwarfs Main sequence ("dwarfs") Subgiants Giants Red
Blue_supergiant
Type of star larger than main-sequence but smaller than a giant
Hertzsprung–Russell diagram Spectral type O B A F G K M L T Brown dwarfs White dwarfs Red dwarfs Subdwarfs Main sequence ("dwarfs") Subgiants Giants Red
Subgiant
Frequencies of light emitted by atoms or chemical compounds
spaced groups of many different spectral lines, known as spectral bands. Unresolved band spectra may appear as a spectral continuum. Light consists of electromagnetic
Emission_spectrum
Stellar classification
helium, strong lines of other ionised elements, and hydrogen and neutral helium lines weaker than spectral type B. Stars of this type are very rare, but because
O-type_star
Extension of the Bohr model
of circular (as in Bohr's model of the atom), the fine-structure of the hydrogen atom can be described. The Bohr–Sommerfeld model added to the quantized
Bohr–Sommerfeld_model
Change in a molecule's spectral band position to a longer wavelength
(chrōma) 'color'; hence less common alternate spelling "bathychromic") is a change of spectral band position in the absorption, reflectance, transmittance, or emission
Bathochromic_shift
Brightest star in the constellation Orion
for B8 stars is estimated from the strength and narrowness of the hydrogen spectral lines, and Rigel is assigned to the bright supergiant class Ia. Variations
Rigel
Concept relating to waves and signals
spectrum means "image" or "apparition", including the meaning "spectre". Spectral evidence is testimony about what was done by spectres of persons not present
Spectrum_(physical_sciences)
Young stars of spectral types A and B
star of spectral types A or B. These stars are still embedded in gas-dust envelopes and are sometimes accompanied by circumstellar disks. Hydrogen and calcium
Herbig_Ae/Be_star
Topics referred to by the same term
malignancy ("blood cancer") Hotline, a telecommunications link Hydrogen line, a spectral line Hypotenuse Leg, a postulate of geometry HL, an amateur radio
HL
German spectroscopist (1841–1913)
spectroscopy, leading eventually to the discovery of the hydrogen spectral lines series (Lyman series) by Theodore Lyman in 1914. Lyman, T. (1914), "Victor
Victor_Schumann
Continuous band of stars that appears on plots of stellar color versus brightness
assigning a different letter to each star based on the strength of the hydrogen spectral line before the relationship between spectra and temperature was known
Main_sequence
the liquid, rotations tend to be restricted by hydrogen bonds, giving the librations. Also, spectral lines are broader causing overlap of many of the
Electromagnetic absorption by water
Electromagnetic_absorption_by_water
White dwarf whose luminosity is variable
stars, with hydrogen-dominated atmospheres and the spectral type DA; DBV, or V777 Her, stars, with helium-dominated atmospheres and the spectral type DB;
Pulsating_white_dwarf
Star that has little or no hydrogen in its atmosphere
the hydrogen lines are very faint and of the same intensity as the additional dark lines”. In 1906, Hans Ludendorff found that Hγ Balmer spectral lines
Hydrogen-deficient_star
Astronomical spectroscopic term
For a neutral hydrogen atom, spectral lines are formed when an electron transitions between energy levels. The Lyman series of spectral lines are produced
Lyman-alpha_forest
Low frequency radio telescope in South Africa
look at the fraction of hydrogen that is ionized. Astronomers observe cold atomic hydrogen with the 21 cm (1420 MHz) spectral line. Assuming that reionization
Hydrogen Epoch of Reionization Array
Hydrogen_Epoch_of_Reionization_Array
Type of chemically peculiar star
solely from hydrogen lines is intermediate. This leads to two or three spectral types being given. For example, Sirius has been given a spectral type of kA0hA0VmA1
Am_star
Main-sequence star of spectral type O
main-sequence—core hydrogen-burning—star of spectral type O. The spectral luminosity class is V, although class O main sequence stars often have spectral peculiarities
O-type_main-sequence_star
Quasar and Lyman-alpha blob in the constellations of Canes Venatici and Coma Berenices
both NV and CIV emission lines in order to calculate the widths of the Hβ spectral line of at least 29 quasars, including TON 618, as a direct measurement
TON_618
German physicist (1865–1947)
electrical discharges. He is also known for the Paschen series, a series of hydrogen spectral lines in the infrared region that he first observed in 1908
Friedrich_Paschen
Series of lines in atomic spectra
The sharp series is a series of spectral lines in the atomic emission spectrum caused when electrons descend from higher-energy s orbitals of an atom to
Sharp_series
Scatter plot of stars showing the relationship of luminosity to stellar classification
K line and two hydrogen Balmer lines. These spectral lines serve as a proxy for the temperature of the star, an early form of spectral classification
Hertzsprung–Russell_diagram
Substellar object
brown dwarfs do not undergo stable hydrogen fusion, they cool down over time, progressively passing through later spectral types as they age. The "brown"
Brown_dwarf
Concept in theoretical astrophysics
theoretical astrophysics, there can be a sphere of ionized hydrogen (H II) around a young star of the spectral classes O or B. The theory was derived by Bengt Strömgren
Strömgren_sphere
Series of lines in atomic spectra
The fundamental series is a set of spectral lines in a set caused by transition between d and f orbitals in atoms. Originally the series was discovered
Fundamental_series
States of matter for water as a solid
Absorption Spectra of Hydrogen-Ordered Ice: a Step to the Exploration of Ice XI in Space". The Astrophysical Journal Supplement Series. 184 (2): 361–365.
Phases_of_ice
Excited atomic quantum state with high principal quantum number (n)
electric potential looks identical to that experienced by the electron in a hydrogen atom. In spite of its shortcomings, the Bohr model of the atom is useful
Rydberg_atom
Instrument to measure the properties of visible light
elements by their characteristic spectral lines. These lines are named for the elements which cause them, such as the hydrogen alpha, beta, and gamma lines
Optical_spectrometer
Mössbauer August Herman Pfund (1879–1949), discovered the Pfund hydrogen spectral series. Max Planck (1858–1947) Bill Price Aleksandr Mikhailovich Prokhorov
List_of_spectroscopists
Statistical task that deconstructs a time series into several components
Hilbert–Huang transform Least squares Least-squares spectral analysis Stochastic drift Trend filtering "6.1 Time series components | OTexts". www.otexts.org. Retrieved
Decomposition_of_time_series
Stars with a supergiant luminosity class with a spectral type of K or M
burning hydrogen in their cores, with masses between 10 and 30 or 40 M☉ will have temperatures between about 25,000K and 32,000K and spectral types of
Red_supergiant
Device for producing coherent EM waves in the sub-visible spectrum
Astrophysical Gas". Atoms, Ions and Molecules: New Results in Spectral Line Astrophysics, ASP Conference Series (ASP: San Francisco). 16: 163. Bibcode:1991ASPC..
Maser
Spectral features due to inelastic interactions
In spectroscopy, collision-induced absorption and emission refers to spectral features generated by inelastic collisions of molecules in a gas. Such inelastic
Collision-induced absorption and emission
Collision-induced_absorption_and_emission
Swedish physicist (1854–1919)
Balmer's, who presented an empirical formula for the visible spectral lines of the hydrogen atom in 1885. However, Rydberg's research led him to publish
Johannes_Rydberg
Technique to analyze the infrared spectrum of matter
gaseous material. An FTIR spectrometer collects high-resolution spectral data over a wide spectral range, from the near- to far-IR region. This confers a significant
Fourier-transform infrared spectroscopy
Fourier-transform_infrared_spectroscopy
'diffuse', and 'sharp' series. Rydberg gave a formula for wave-numbers of all spectral series of all the alkalis and hydrogen. In 1895, the German physicist
History_of_spectroscopy
Isotope of hydrogen with one neutron
Deuterium (hydrogen-2, symbol 2H or D, also known as heavy hydrogen) is one of two stable isotopes of hydrogen; the other is protium, or hydrogen-1, 1H. The
Deuterium
Principle of spectral lines
the relationship of the spectral lines for all atoms, as a generalization of an earlier rule by Johannes Rydberg for the hydrogen atom and the alkali metals
Rydberg–Ritz combination principle
Rydberg–Ritz_combination_principle
Method of identifying trace chemicals
Mass spectral interpretation is the method employed to identify the chemical formula, characteristic fragment patterns and possible fragment ions from
Mass_spectral_interpretation
Details in the emission spectrum of an atom
In atomic physics, the fine structure describes the splitting of the spectral lines of atoms due to electron spin and relativistic corrections to the non-relativistic
Fine_structure
Rare star with tremendous luminosity and high rates of mass loss by stellar winds
their spectral lines, producing a distinctive spectral shape known as a P Cygni profile. The use of hydrogen emission lines is not helpful for defining the
Hypergiant
Visible, gaseous part of a fire
typically being black-body radiation and spectral band emission, with both spectral line emission and spectral line absorption playing smaller roles. In
Flame
Galaxy in the constellation Pegasus
of nucleus that is defined by its spectral line emission which has weakly ionized or neutral atoms, while the spectral line emission from strongly ionized
NGC_7769
Exoplanet orbiting 82 G. Eridani
therefore one of the nearest stars. The star has a spectral type of G8V, which is similar to the Sun's spectral type of G2V. The luminosity class "V" classifies
HD_20794_d
Type of large cool star
Hertzsprung–Russell diagram Spectral type O B A F G K M L T Brown dwarfs White dwarfs Red dwarfs Subdwarfs Main sequence ("dwarfs") Subgiants Giants Red
Red_giant
Open star cluster in the constellation Cassiopeia
are spectral class B stars that show prominent emission lines of hydrogen in their spectrum. Most of the Be stars in the cluster lie between spectral class
NGC_663
fluoride laser Hydrogen ion Hydrogen ion cluster Hydrogen line Hydrogen maser Hydrogen silsesquioxane Hydrogen spectral series Hydrophone Hydropower Hydrostatic
Index_of_physics_articles_(H)
Topics referred to by the same term
Massachusetts, United States, a school from c. 1884 to c. 1971 Lyman series of hydrogen spectral lines in physics Lyman Block, Brockton, Massachusetts United
Lyman
Matter and radiation in the space between the star systems in a galaxy
was once thought to be a new element, nebulium. Spectral lines from highly excited states of hydrogen are detectable at infra-red and longer wavelengths
Interstellar_medium
Feature observed in spectroscopy
Spectral line shape or spectral line profile describes the form of an electromagnetic spectrum in the vicinity of a spectral line – a region of stronger
Spectral_line_shape
Triple star system in the constellation Tucana
dramatically so that it appeared as a B hypergiant with prominent hydrogen spectral lines. Since then it has returned to near its original brightness
HD_5980
Low-mass supergiant that is almost devoid of hydrogen
broader category of hydrogen-deficient stars. The latter includes cool carbon stars like R Coronae Borealis variables, helium-rich spectral class O or B stars
Extreme_helium_star
Type of cool giant star
variables, show strong hydrogen emission lines. The Hβ emission is often unusually strong compared to other lines of the Balmer series in a normal M star
S-type_star
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