Fraunhofer lines

Fraunhofer Lines
Related Category: Astronomy: General
(froun´hõfr): see sun.
More on Fraunhofer Lines
Sun - intensely hot, self-luminous body of gases at the center of the solar system.

Fraunhofer lines The collection of over 600 absorption lines in the spectrum of the Sun, first categorized by Joseph Fraunhofer in 1812.
frequency The number of wave crests passing any given point per unit of time.

Fraunhofer Lines
Fraunhofer was the inventor of the diffraction grating. He assigned letters to the black absorption lines in the Solar Spectrum.

Fraunhofer Lines- the dark lines in the spectrum of the sun
Frequency- for a wave, the number of complete cycles per second ...

FRAUNHOFER LINES

Strong spectral lines in the solar spectrum labelled with the letters A to K by Joseph Fraunhofer in early nineteenth century.

Fraunhofer lines. Dark absorption lines seen in the spectrum of the Sun.

Fraunhofer Lines
(a) The dark lines in the spectrum of light from the Sun, caused by the absorption of particular wavelengths by certain elements in its cooler outer regions.

Fraunhofer lines - (n.)
The absorption lines of a solar or other stellar spectrum.
frequency - (n.) ...

Fraunhofer lines (NASA Thesaurus / NASA SP-7, 1965) Dark lines in the absorption spectrum of solar radiation due to absorption by gases in the outer portions of the sun and in the earth's atmosphere.

telluric lines Absorption lines in a solar spectrum produced by constituents of the atmosphere of the earth itself rather than by gases in the outer solar atmosphere such as those responsible for the Fraunhofer lines.

He thus caught a preliminary glimpse of the " Fraunhofer lines," so called because ofer Joseph Fraunhofer brought them into prominent ofer notice by the diligence and insight of his labours upon them in 1814-1815.

Sun's Spectrum showing Fraunhofer lines
Two key questions arise from studying these lines - what do they represent and how are they formed? The solutions to these questions were to take some time.

The ones noted first were dark lines (named Fraunhofer lines after their discoverer), suggesting increased absorption of light, not increased emission.

Dark absorption lines in the sun's spectrum and that of other stars are called Fraunhofer lines after Joseph von Fraunhofer (1787-1826) who observed them in 1817.

The optical window allows through visible light, from red, as far as the A band (see Fraunhofer lines) of molecular oxygen (O2) at 7600 Å, to violet and a little beyond, as far as at the ozone (O3) cut-off at 2950 Å.

Kirchhoff had explained the Sun's Fraunhofer lines - the dark lines in the solar spectrum (the light from the Sun) were the same as the emission lines observed by various heated chemical substances. Kirchhoff realized that the Sun was hot and gaseous.

The precise origin of these 'Fraunhofer lines' as we call them today remained in doubt for many years, until Gustav Kirchhoff, in 1859, ...

One of about a dozen of the strongest Fraunhofer lines seen in the Solar spectrum, the A band at 7600 angstoms is due to telluric lines of molecular oxygen in the Earth's atmosphere.
A-coefficient ...

In the early 1800s, he observed that the continuous spectrum was marred by over 700 dark lines (now called Fraunhofer lines). Fraunhofer's work with the spectra and also with diffraction gratings was seminal in the science of spectroscopy.

Amplitude
Angular frequency
Frequency
Fraunhofer lines, spectral lines traditionally used as standard optical wavelength references
Periodic function
Wavevector ...

Joseph von Fraunhofer (b. March 6, 1787, Straubing, Bavaria [Germany]--d. June 7, 1826, Munich), German physicist who first studied the dark lines of the Sun's spectrum, now known as Fraunhofer lines.

Extremely high resolution spectrum of the Sun showing thousands of elemental absorption lines (Fraunhofer lines)
[edit] Nature of excitation measured ...

High resolution spectrum of the Sun showing thousands of elemental absorption lines (fraunhofer lines).

Many of the Fraunhofer lines in the solar spectrum retain the notations he created to designate them.

scattered by protons and free electrons in the hot outer atmosphere of the Sun. The K corona extends out to about 700,000 km from the photosphere. The K Corona's continuous spectrum resembles the photospheric spectrum, but the Fraunhofer lines are ...

Kirchoff found that when light shines through a gas, the gas absorbs some of the light, the same wavelengths of light that it would emit when heated. He applied his techniques to the Sun, explaining Fraunhofer lines.

See also: Wavelength, Light, Spectrum, Sun, Element