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Glossarbegriffe: Spektrum
Redirected from Spektrograf
Description: Ein Regenbogen entsteht, wenn Wassertröpfchen das Licht in die Spektralfarben Violett, Blau, Grün, Gelb, Orange und Rot zerlegen. Jede Farbe entspricht einem Bereich von Wellenlängen, und die Regenbogenfarben sind in der Reihenfolge zunehmender Wellenlänge von violett bis rot angeordnet. Diese Art von zerlegtem Licht oder allgemeiner von elektromagnetischer Strahlung nach Wellenlängen wird als Spektrum bezeichnet.
Elektromagnetische Strahlung ist eine Mischung aus Lichtteilchen, die "Photonen" genannt werden. Um ein Spektrum (beispielsweise von der Sonne oder von einem anderen astronomischen Objekt) zu erstellen, sortiert man die Photonen nach ihrer Energie und hält fest, wie viele Photonen es in jedem Energiebereich gibt. Nach einem Grundgesetz der Quantenmechanik ist dies gleichbedeutend mit der Sortierung des Lichts nach der Frequenz - eine weitere Möglichkeit, ein Spektrum zu erfassen.
Wenn die Energiemenge gleichmäßig mit der Wellenlänge (oder der Photonenenergie oder der Frequenz) variiert,
wird das Spektrum als kontinuierlich bezeichnet. Im Gegensatz dazu werden scharfe Einbrüche oder Spitzen in einem Spektrum bei bestimmten Wellenlängen als Absorptions- bzw. Emissionslinien bezeichnet. Solche Linien entstehen aufgrund von
Übergängen zwischen verschiedenen Energieniveaus innerhalb von Atomen oder Molekülen (oder sogar Atomkernen), die entweder Strahlung bei bestimmten Wellenlängen absorbieren oder emittieren. Im sichtbaren Licht zeigen Sterne beispielsweise kontinuierliche Spektren mit Absorptionslinien. Diese Linien geben Aufschluss über die chemische Zusammensetzung eines Sterns. Die Analyse von Spektren wird als Spektroskopie bezeichnet; Instrumente, die die Aufnahme von Spektren ermöglichen, werden Spektroskope, Spektrometer oder Spektrographen genannt.
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Term and definition status: The original definition of this term in English have been approved by a research astronomer and a teacher The translation of this term and its definition is still awaiting approval
The OAE Multilingual Glossary is a project of the IAU Office of Astronomy for Education (OAE) in collaboration with the IAU Office of Astronomy Outreach (OAO). The terms and definitions were chosen, written and reviewed by a collective effort from the OAE, the OAE Centers and Nodes, the OAE National Astronomy Education Coordinators (NAECs) and other volunteers. You can find a full list of credits here. All glossary terms and their definitions are released under a Creative Commons CC BY-4.0 license and should be credited to "IAU OAE".
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24 Hours of Rainbow
Bildunterschriften: This panoramic view taken with a smartphone of Livorno, Italy, showcases a series of vivid rainbows captured on three different days in December 2021. Rainbows are the result of sunlight being refracted by water droplets suspended in the air, typically after rainfall or during misty conditions. The water droplets act like a prism, breaking up (refracting) the sunlight into the various colours. The different wavelengths of light are refracted by different amounts, which is why we see this layering of colours. The photographer skillfully merged the most remarkable shots taken on different days to highlight the diverse sizes and brilliance of these rainbows. The locations at which the rainbows appear to be centred are different because each rainbow appeared when the Sun was at a different position in the sky. This composite image beautifully captures the transient yet mesmerising allure of rainbows, illustrating their fleeting appearance and gradual dissipation influenced by the shifting atmospheric conditions.
Bildnachweis: Fabrizio Guasconi/IAU OAE (CC BY 4.0)
Bildnachweis: Fabrizio Guasconi/IAU OAE (CC BY 4.0)
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Related Diagrams
Spectrum of an O-type star
Bildunterschriften: The spectrum of the O-type star HD 235673 with wavelength in nanometers on the x-axis and flux on the y-axis. The top part of the plot shows the same spectrum but with bright patches for wavelengths with high flux and dark patches for wavelengths with low flux. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. For O-type stars the most important features are a small number of lines caused by ionized helium. These lines are stronger in O-type stars than in cooler stars. Lines from helium atoms and hydrogen atoms also appear in the spectrum. The spectrum has more flux at the blue end of the spectrum than at the red end of the spectrum.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Spectrum of a B-type star
Bildunterschriften: The spectrum of the B-type star HD 258982. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. For B-type stars the most important lines are caused by helium atoms. These lines are strongest in B-type stars and weaker in hotter and cooler types. Lines from hydrogen atoms are also present but are not as strong as in cooler A-type stars.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Spectrum of an A-type star
Bildunterschriften: The spectrum of the A-type star BD-11 1212. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. Lines from hydrogen atoms dominate the spectra of A-type stars and are strongest at this spectral type.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Spectrum of an F-type star
Bildunterschriften: The spectrum of the F-type star 2MASS J22243289+4937443. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The lines from hydrogen atoms that are strongest in A-type stars are still relatively strong in F-type stars but lines from metals, particularly ionised calcium begin to become strong at this spectral type.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Spectrum of a G-type star
Bildunterschriften: The spectrum of the G-type star UCAC4 700-069569. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. In G-type stars lines from hydrogen atoms are weaker than in F-type stars and lines from ionised calcium stronger. Lines from metal atoms such as atoms of iron, sodium and calcium also begin to become prominent.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Spectrum of a K-type star
Bildunterschriften: The spectrum of the K-type star 2MASS J19554455+4754531. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The spectra of K-type stars are dominated by metal atoms such as iron, sodium and calcium atoms. There are so many lines from metal atoms, far too many to mark individually, that the spectrum has a choppy, ragged appearance. The lines of hydrogen atoms and calcium ions are much weaker than in the hotter G-type stars.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Spectrum of an M-type star
Bildunterschriften: The spectrum of the M-type star 2MASS J15581272+8457104. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The black lines show spectral absorption lines caused by atoms, ions and molecules of different elements in the star’s atmosphere. These atoms, ions and molecules absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The atmospheres of M-type stars are cool enough for some chemical compounds to form. These are often referred to as molecules in astronomy, even if they are not strictly molecules in chemistry. These molecules produce so many lines in an M-type star’s spectrum that the lines appear to merge together in huge bands that remove large chunks from the spectrum. In M-type stars, titanium oxide has a large number of these bands in visible light, dominating huge regions of the spectrum.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Stellar spectral types
Bildunterschriften: The spectra of seven stars ordered by spectral type ranging from the hottest (O-type) at the top to the coolest (M-type at the bottom). The x-axis shows the wavelength of light and the y-axis is a measure of the flux of light received at that wavelength. Each spectrum is normalized (the flux at each wavelength is divided by the maximum flux in that spectrum) and the spectra are then offset from each other along the y-axis to make the plot easier to view. The colour of the lines between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The hotter stars have more of their flux at the bluer end of the spectrum and the cooler stars have more of their flux at the redder end. However the total amount of flux a star emits depends on its size and temperature. Due to this, a hot star will emit more red light than a cool star of the same size even if the cool star emits almost all its light in red light but this is not visible in this plot due to the normalization mentioned above. The sharp, narrow drops in the spectra are absorption lines caused by atoms and ions in the stars’ atmospheres. The strength of a spectral line depends on the temperature of a star’s atmosphere. Take the hydrogen line at 656.5 nm as an example. All of the stars in this plot are primarily made of hydrogen, but the 656.5 nm hydrogen line is weak for the hottest and coolest stars but strongest for spectral types A and F. This is because hydrogen absorbs more light at 656.5 nm at the temperatures of A and F stars’ atmospheres than in hotter or cooler stars.
The coolest star here, the M-type star, has wide absorption bands in its spectra. This is because this star is cool enough to have compounds such as titanium oxide in its atmosphere. These compounds, often called molecules in astronomy, produce wider spectral absorption features than atoms or ions.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Stellar spectral types - bands
Bildunterschriften: The spectra of seven stars ordered by spectral type ranging from the hottest (O-type) at the top to the coolest (M-type at the bottom). The x-axis shows the wavelength of light while the brightness or darkness at each wavelength corresponds to the flux of light received from the star at that wavelength with darker patches having less flux and brighter patches more. Each spectrum is normalized (the flux at each wavelength is divided by the maximum flux for that spectrum) so that the maximum flux should appear with the same brightness for all the spectra. The colour plotted between 400 nm and 700 nm roughly corresponds to the color the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively.
The hotter stars have more of their flux at the bluer end of the spectrum and the cooler stars have more of their flux at the redder end. However the total amount of flux a star emits depends on its size and temperature. Due to this, a hot star will emit more red light than a cool star of the same size even if the cool star emits almost all its light in red light but this is not visible in this plot due to the normalization mentioned above. The dark, narrow patches in the spectra are absorption lines caused by atoms and ions in the stars’ atmospheres. The strength of a spectral line depends on the temperature of a star’s atmosphere. Take the hydrogen line at 656.5 nm as an example. All of the stars in this plot are primarily made of hydrogen, but the 656.5 nm hydrogen line is weak for the hottest and coolest stars but strongest for spectral types A and F. This is because hydrogen absorbs more light at 656.5 nm at the temperatures of A and F stars’ atmospheres than in hotter or cooler stars.
The coolest star here, the M-type star, has wide absorption bands in its spectra. This is because this star is cool enough to have compounds such as titanium oxide in its atmosphere. These compounds, often called molecules in astronomy, produce wider spectral absorption features than atoms or ions.
Bildnachweis: IAU OAE/SDSS/Niall Deacon
Bildnachweis: IAU OAE/SDSS/Niall Deacon
License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
Related Activities
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astroEDU educational activity (links to astroEDU website) Description: Learn about light and spectra building a spectroscope with a CD!License: CC-BY-4.0 Creative Commons Namensnennung 4.0 International (CC BY 4.0) icons
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Find the hidden rainbows
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