stellar spectrum

collocation in English

meaningsofstellarandspectrum

These words are often used together. Click on the links below to explore the meanings. Or,see other collocations withspectrum.
stellar
adjective
uk
/ˈstel.ər/us
/ˈstel.ɚ/
of a star ...
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spectrum
noun[C]
uk
/ˈspek.trəm/us
/ˈspek.trəm/
the set of colours into which a beam of light can be separated, or a range of waves, such as light waves or ...
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(Definition ofstellarandspectrumfrom theCambridge English Dictionary© Cambridge University Press)

Examplesofstellar spectrum

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The quality of the retrieved spectra is significantly more affected by noise than thestellarspectrum.
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By studying the high-resolutionstellarspectrumcarefully, one can detect elements present in the planet's atmosphere.
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The third component, the heliocentric radial velocity, can be measured by the average red-shift (or blue-shift) of thestellarspectrum.
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Using thestellarspectrum, astronomers can also determine the surface temperature, surface gravity, metallicity and rotational velocity of a star.
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This is a single-lined spectroscopic binary system wherein the presence of a companion object is revealed by shifts in thestellarspectrum.
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A typicalstellarspectrumwill consist of a continuum, containing absorption lines, each of which is attributed to a particular atomic energy level transition in the atmosphere of the star.
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His primary interest was the study of stellar spectra.
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His main contributions was in the study of solar and stellar spectra.
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A transmission grism is a useful component in an astronomical telescope, allowing observation of stellar spectra.
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This equation has been widely applied to the interpretation of stellar spectra, which are characteristic of the chemical composition of the light source.
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First he applied it to the solar chromosphere, then to stellar spectra.
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The divergences with the straight line are due to the absortions and emission lines in the stellar spectra.
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There he developed an interest in stellar spectra using photography.
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The original code simulated stellar spectra assuming the atmosphere to be in hydrostatic equilibrium, plane parallel, with convection described by mixing-length theory.
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Schuster formulated in 1905 a problem in radiative transfer in an attempt to explain the appearance of absorption and emission lines in stellar spectra.
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They can not be identified in stellar spectra.
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These examples are from corpora and from sources on the web. Any opinions in the examples do not represent the opinion of the Cambridge Dictionary editors or of Cambridge University Press or its licensors.
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