Spectral line: Wikis

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Continuous spectrum
Emission lines
Absorption lines

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, compared with the nearby frequencies.

Contents

Types of line spectra

Spectral lines are the result of interaction between a quantum system (usually atoms, but sometimes molecules or atomic nuclei) and a single photon. When a photon has about the right amount of energy to allow a change in the energy state of the system (in the case of an atom this is usually an electron changing orbitals), the photon is absorbed. Then it will be spontaneously re-emitted, either in the same frequency as the original or in a cascade, where the sum of the energies of the photons emitted will be equal to the energy of the one absorbed (assuming the system returns to its original state). The direction and polarization of the new photons will, in general, correlate with those of the original photon.

Depending on the type of gas, the photon source and what reaches the detector of the instrument, either an emission line or an absorption line will be produced. If the gas is between the photon source and the detector, a decrease in the intensity of light in the frequency of the incident photon will be seen, as the reemitted photons will mostly be in directions different from the original one. This will be an absorption line. If the detector sees the gas, but not the original photon source, then the detector will see the photons reemitted in a narrow frequency range. This will be an emission line.

Spectral lines are highly atom-specific, and can be used to identify the chemical composition of any medium capable of letting light pass through it (typically gas is used). Several elements were discovered by spectroscopic means, such as helium, thallium, and cerium. Spectral lines also depend on the physical conditions of the gas, so they are widely used to determine the chemical composition of stars and other celestial bodies that cannot be analyzed by other means, as well as their physical conditions.

Isomer shift is the displacement of an absorption line due to the absorbing nuclei having different s-electron densities from that of the emitting nuclei.

Mechanisms other than atom-photon interaction can produce spectral lines. Depending on the exact physical interaction (with molecules, single particles, etc.) the frequency of the involved photons will vary widely, and lines can be observed across the electromagnetic spectrum, from radio waves to gamma rays.

Nomenclature

Spectral lines often have a unique Fraunhofer line designation, such as K for a line at 410.175 nm emerging from singly ionized Ca+. In other cases the lines are designed according to the level of ionization adding a roman number to the designation of the chemical element, so that Ca+ also have the designation CaII. Neutral atoms are denoted with the roman number I, singly ionized atoms with II, and so on, so that for example FeIX represents eight times (IX, roman 9) ionized iron.

Spectral line broadening and shift

A spectral line extends over a range of frequencies, not a single frequency (i.e., it has a nonzero linewidth). In addition, its center may be shifted from its nominal central wavelength. There are several reasons for this broadening and shift. These reasons may be divided into two broad categories - broadening due to local conditions and broadening due to extended conditions. Broadening due to local conditions is due to effects which hold in a small region around the emitting element, usually small enough to assure local thermodynamic equilibrium. Broadening due to extended conditions may result from changes to the spectral distribution of the radiation as it traverses its path to the observer. It also may result from the combining of radiation from a number of regions which are far from each other.

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Broadening due to local effects

  • Thermal Doppler broadening: The atoms in a gas which are emitting radiation will have a distribution of velocities. Each photon emitted will be "red"- or "blue"-shifted by the Doppler effect depending on the velocity of the atom relative to the observer. The higher the temperature of the gas, the wider the distribution of velocities in the gas. Since the spectral line is a combination of all of the emitted radiation, the higher the temperature of the gas, the broader will be the spectral line emitted from that gas. This broadening effect is described by a Gaussian profile and there is no associated shift.
  • Pressure broadening: the presence of nearby particles will affect the radiation emitted by an individual particle. There are two limiting cases by which this occurs:
  • Impact pressure broadening: The collision of other particles with the emitting particle interrupts the emission process. The duration of the collision is much shorter than the lifetime of the emission process. This effect depends on both the density and the temperature of the gas. The broadening effect is described by a Lorentzian profile and there may be an associated shift.
  • Quasistatic pressure broadening: The presence of other particles shifts the energy levels in the emitting particle, thereby altering the frequency of the emitted radiation. The duration of the influence is much longer than the lifetime of the emission process. This effect depends on the density of the gas, but is rather insensitive to temperature. The form of the line profile is determined by the functional form of the perturbing force with respect to distance from the perturbing particle. There may also be a shift in the line center.
Pressure broadening may also be classified by the nature of the perturbing force as follows:
  • Linear Stark broadening occurs via the linear Stark effect which results from the interaction of an emitter with an electric field, which causes a shift in energy which is linear in the field strength. (\Delta E \sim 1/r^2)
  • Resonance broadening occurs when the perturbing particle is of the same type as the emitting particle, which introduces the possibility of an energy exchange process. (\Delta E \sim 1/r^3)
  • Quadratic Stark broadening occurs via the quadratic Stark effect which results from the interaction of an emitter with an electric field, which causes a shift in energy which is quadratic in the field strength. (\Delta E \sim 1/r^4)
  • Van der Waals broadening occurs when the emitting particle is being perturbed by van der Waals forces. For the quasistatic case, a van der Waals profile[note 1] is often useful in describing the profile. The energy shift as a function of distance is given in the wings by e.g. the Lennard-Jones potential (\Delta E \sim 1/r^6).

Notes:

  1. ^ "van der Waals profile" appears as lowercase in almost all sources, such as: Statistical mechanics of the liquid surface by Clive Anthony Croxton, 1980, A Wiley-Interscience publication, ISBN 0471276634, 9780471276630, [1]; and in Journal of technical physics, Volume 36, by Instytut Podstawowych Problemów Techniki (Polska Akademia Nauk), publisher: Państwowe Wydawn. Naukowe., 1995, [2]

Broadening due to non-local effects

Certain types of broadening are the result of conditions over a large region of space rather than simply upon conditions that are local to the emitting particle.

  • Opacity broadening: Electromagnetic radiation emitted at a particular point in space can be absorbed as it travels through space. This absorption depends on wavelength. The line is broadened because photons at the line wings have a smaller reabsorption probability than photons at the line center. Indeed, the absorption near line center may be so great as to cause a self reversal in which the intensity at the center of the line is less than in the wings.
  • Macroscopic Doppler broadening: Radiation emitted by a moving source is a subject to the Doppler shift due to a finite line-of-sight velocity projection. If different parts of the emitting body have different velocities (along the line of sight), the resulting line will be broadened, with the line width proportional to the width of the velocity distribution. For example, radiation emitted from a distant rotating body, such as a star, will be broadened due to the line-of-sight variations in velocity on opposite sides of the star. The greater the rate of rotation, the broader the line. Another example is an imploding plasma shell in a Z-pinch.

Combined effects

Each of these mechanisms can act in isolation or in combination with others. Assuming each effect is independent, the observed line profile is a convolution of the line profiles of each mechanism. For example, a combination of the thermal Doppler broadening and the impact pressure broadening yields a Voigt profile.

However, the different line broadening mechanisms are not always independent. For example, the collisional effects and the motional Doppler shifts can act in a coherent manner, resulting under some conditions even in a collisional narrowing, known as the Dicke effect.

See also

Notes

  1. ^ For example, in the following article, decay was suppressed via a microwave cavity, thus reducing the natural broadening: Gabrielse, Gerald; H. Dehmelt (1985). "Observation of Inhibited Spontaneous Emission". Physical Review Letters 55 (1): 67–70. doi:10.1103/PhysRevLett.55.67. PMID 10031682.  

References

  • Griem, Hans R. (1997). Principles of Plasmas Spectroscopy. Cambridge: University Press. ISBN 0-521-45504-9.  
  • Griem, Hans R. (1974). Spectral Line Broadening by Plasmas. New York: Academic Press. ISBN 0-12-302850-7.  
  • Griem, Hans R. (1964). Plasma Spectroscopy. New York: McGraw-Hill book Company.  

Simple English

File:Spectral lines
Continuous spectrum
File:Spectral lines
Emission lines
File:Spectral lines
Absorption lines

Spectral lines are how scientists tell one element from another by looking at color.

The colors of the rainbow

In order to understand spectral lines, color has to be understood. In a rainbow, the colors of light go from purple to red. Several hundred years ago, the famous scientist Issac Newton did an experiment where he showed that even white light from the Sun was made up of all the colors of the rainbow. When other scientists following him looked at this rainbow very closely, they noticed that there were dark lines breaking up the rainbow, where certain shades of colors should be. These lines were very small, and could only be seen when the rainbow got streched out very far. They investigated this further, and discovered that certain chemical elements, like the hydrogen and helium that make up the Sun, absorbed certain frequencies of light where those colors should be, like a sponge absorbs water, but does not absorb chalk.

Elemental fingerprints

Soon, scientists discovered that when they heated up other chemical elements, like calcium and oxygen, so hot that they shined with a white light, they found similar lines, but in different places. No two chemical elements had these lines in exactly the same places along the rainbow, and they also soon discovered that could be used to be able to tell what stars were made up of in the Universe.

The reason the chemical elements can do this is because of the number and places of electrons orbiting around the center of each atom of each chemical element. These electrons, when light hits them, absorb a specific wavelength, or color of light, and what color they absorb depend on their position around the atom. Since each chemical element has a certain number of electrons, each chemical element has this unique set of spectral lines.

Red shift

Since each set of spectral lines was unique, scientists could also be able to use this in a technique called red shift. Red shift is a method astronomers use, after they know what a star is made of, to tell how fast an object far away in the Universe is moving. It also tells them how far away it is, .


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