Spectral Line
A spectral line is like a fingerprint that can be used to identify the atoms, elements or molecules present in a star, galaxy or cloud of interstellar gas.
Spectral line
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Definition: spectral line: Light given off at a specific frequency by an atom or molecule.
Spectral line
Wikipedia, the free encyclopedia - Cite This Source
A spectral line is a dark or bright line in an otherwise uniform and continuous spectrum, resulting from an excess or deficiency of photons in a narrow frequency range, ...
spectral line
a particular wavelength of light corresponding to the energy transition of a specific atom or molecule
spectral type ...
Spectral line: Light given off at a specific frequency by an atom or molecule. Every different type of atom or molecule gives off light at its own unique set of frequencies.
Spectral Line
a line in a spectrum due to the emission or absorption of electromagnetic radiation at a discrete wavelength. Spectral lines result from discrete changes in the energy of an atom or molecule.
Spectral Lines
(a) Dark lines visible in an absorption spectrum, or bright lines that make up an emission spectrum.
Spectral line A narrow range of spectral color, emitted (or absorbed) by a specific atom (or molecule).
SPECTRAL LINE
A spectral line is a bright or dark line found in the spectrum of some radiant source. Bright lines indicate emission, dark lines indicate absorption.
spectral line A radiative feature observed in emission (bright) or absorption (dark) at a specific frequency or wavelength.
Spectral Line
In a spectrum, an emission (bright) or absorption (dark) at a specific frequency or wavelength.
Star ...
Spectral lines or bands that originate from absorption by gases such as O2, H2O, or CO2 in the Earth's atmosphere. [H76]
Tellurium ...
Spectral line
A spectral line is a dark or bright line in an otherwise uniform and continuous optical spectrum, resulting from an excess or deficiency of photons in a narrow frequency range, compared with the nearby frequencies....
emission.
Spectral lines also result from vibrational and rotational transitions of such interstellar molecules as water vapor (H2O), ammonia (NH3), formaldehyde (H2CO), and carbon monoxide (CO).
Spectral lines occur throughout the entire electromagnetic spectrum. Usually, electron transitions among the lowest orbitals of the lightest elements (such as hydrogen and helium) produce visible and ultraviolet spectral lines.
Spectral lines in the UV spectrum of hydrogen produced by transitions whose lowest orbit of electrons is at ground state (Lyman). Spectral lines in the visible and near UV of hydrogen produced by transitions whose lowest orbit is second (Balmer).
- spectral line - Space and Astronomy Definition - Online Dictionary and Glossary Definition of spectral line
- Markov Transition Matrix - Glossary - Dictionary Definition of Markov Transition Matrix
- Rydberg State - definition of Rydberg state ...
The spectral lines seen are those expected to be common at 6,000 K, where the thermal energy of each particle is about 0.5 volt.
If the spectral lines in a star's spectrum are uniformly redshifted this would indicate relative recessional motion between the observer and the star. The amount of redshift would depend on the recession velocity.
Although spectral lines of many elements are present with widely varying strengths, the differences among the spectra in Figure 17.12 are not due to differences in composition.
Carbon II spectral line intensity profiles showing that carbon is abundant in many regions of space.
Observation: spectral lines from the top layer of white dwarfs are significantly shifted by an amount predicted for compact solar-mass objects.
21-cm line - A spectral line of neutral hydrogen at the radio wavelength of of 21 cm.
spectral line (Imagine the Universe Dictionary - NASA GSFC) Light given off at a specific frequency by an atom or molecule.
Lyman series: Spectral lines in the ultraviolet spectrum of hydrogen produced by transitions whose lowest orbit is the ground state.
The wavelength of a spectral line as measured in a laboratory, when there is no relative motion between source and observer.
retrograde motion - (n.) ...
Stark effect The broadening or splitting of a spectral line observed when a luminous gas is acted upon by a strong electric field.
stellar classification Stars given a designation consisting of a letter and a number according to the nature of their spectral lines which corresponds roughly to surface temperature.
1860 - Gustav Kirchhoff and Robert Bunsen discover that each chemical element has its own distinct set of spectral lines and use this fact to explain the solar dark lines
1861 - F.G.W.
In addition, measurements of the Doppler effect in the spectral lines show that there is a vortex motion in sunspots similar to that of a tornado on earth.
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).
One reason is that the strength of spectral lines from molecules is related to how asymmetric the molecule is. Since the hydrogen molecule is perfectly symmetric (containing two H atoms), its spectral lines are extremely weak.
Solar flares are often observed using filters to isolate the light emitted by hydrogen atoms in the red region of the solar spectrum (the H-alpha spectral line).
Capella Ab is a yellow-orange giant star of spectral and luminosity type G1 III, with rotationally broadened spectral lines.
The luminosity classes are defined spectroscopically by the width of the observed spectral lines. Big stars have lower atmospheric pressure so the atoms in such an atmosphere are not jostled around as much as in a high pressure atmosphere.
The Tully-Fisher Relation is a correlation between the luminosity of spiral and irregular galaxies and their rate of rotation (rotational velocity, which is measured from the broadening of its spectral lines since the light from it is both red- and ...
Stars are classified by their spectral lines well before we know that those lines are also related to the temperature. The classes of spectral lines are called the spectral types, from O to M.
This scheme measures the shape and nature of certain spectral lines to measure surface gravities of stars.
Bohr's ideas gave an accurate formula for the frequency of spectral lines in many cases and were an enormous help in the codification and understanding of spectra.
Now, remember the Doppler effect, and you will understand why the spectral lines caused by absorption of one gas cloud will be shifted from those caused by absorption from a second cloud, and so on.
These stars are divided into three groups: those with predominantly silicon spectral lines, those with manganese, and those with chromium-strontium lines. Epsilon Ursae Majoris shows a strong chromium line.
Radial velocity is measured by the doppler shift of the star's spectral lines, and is given in units of km/s. The proper motion of a star is determined by precise astrometric measurements in units of milli-arc seconds (mas) per year.
All the stars in this universe are divided in to spectral classes based on their spectral lines. There are 10 spectral classes. The spectral class of a star and the temperature of a star are related.
Redshift: The shift of spectral lines towards the red end of the spectrum when the light source is moving away.
Rhea: Moon of Saturn.
Rocky planet: An Earth-like planet, made of rock rather than ice. Generally smaller planets are rocky.
From the shapes and depths of spectral lines, the astronomer can calculate fundamental qualities of a star, such as how fast the gases churn through the stellar atmosphere or the star's effective temperature.
blueshift
An apparent shift toward shorter wavelengths of spectral lines in the radiation emitted by an object caused by motion between the object and the observer which decreases the distance between them. See also Doppler effect.
Radial motion is motion towards or away from the observer. Radial velocity can be determined using the . Motion towards the observer shifts spectral lines towards the blue; motion away from the observer shifts spectral lines towards the red.
These proportions are determined by studies of the spectral lines in astronomical objects and are averaged for many stars in our cosmic neighborhood.
These motions across the sky combined with their motions along the line of sight (from the doppler shift of spectral lines) give their space motions.
Zeeman Effect - The splitting of a spectral line into two or more components when the atoms or molecules emitting the line are located in a magnetic field
Zenith - The point on the celestial sphere directly above an observer ...
The scientists conclude that Achernar must either rotate faster (and hence, closer to the "critical" (break-up) velocity of about 300 km/sec) than what the spectral observations show (about 225 km/sec from the widening of the spectral lines) or it ...
Each atom has a unique fingerprint because each can only emit or absorb certain wavelengths of energy. Thus, the fingerprint -- as seen in the location and spacing of spectral lines -- is unique for each atom.
To understand how an initially spherical star can create such intricate nebula, PACs takes images in spectral lines to see how the wind from the star shapes the nebula in three dimensions.
Looking through the historical record of stellar spectrographic plates in an attempt to find anomalous spectral lines that may signify a laser beacon signal.
SETI ...
It is a great double star for those with binoculars or small telescopes. It is a peculiar star in that it's spectral lines are variable. There are strong lines of strontium, silicon, and chromium which show a variation in strength over time.
The names of the stars are indicated on the right - most are just their catalog designations. Note how the spectral line patterns change with changing temperature. Click on the image to see a larger version. Image courtesy of NOAO/AURA/NSF.
their high-resolution results in the form of X-Y graphic plots, whose peaks and valleys reveal intensity (brightness) on the vertical axis versus wavelength along the horizontal. Peaks of high intensity on such a plot represent bright spectral lines ...
[Note that the ionization stage is denoted as N0, N+,N++, while the associated spectral lines would be N I, N II, N III, along with brackets if they're so-called forbidden transitions from metastable upper levels.
 See also: Light, Sun, Earth, Spectrum, Solar
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