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Its system of classifying stars by their spectra, or the wavelengths of light they emit, is still in wide use.
Their masses, determined from the extent of the X-ray images and their spectra, ranged from 100 trillion Suns to a quintillion Suns.
As a consequence, their colours rather than their spectra must be measured.
Many central stars are known from their spectra to be very hot.
Their speeds (as determined from the redshifted wavelengths in their spectra) are generally proportional to their distances.
Type I supernovae can be divided into three subgroups Ia, Ib, and Ic on the basis of their spectra.
Their spectra typically show strong lines of metals such as manganese, titanium, iron, chromium, and the lanthanides (also called rare earths), which vary periodically in intensity.
By making the laser cavity part of a reacting flow system, the presence of paramagnetic reaction intermediates can be detected and their spectra recorded.
The best distance determinations are from spectroscopic parallaxes of individual stars i.e., estimates of their absolute magnitudes made from studies of their spectra.
They can be distinguished by the fact that type II have hydrogen features in their spectra, while type I do not.
In order to distinguish brown dwarfs from stars of the same temperature, one can search their spectra for evidence of lithium (which stars destroy when hydrogen fusion begins).
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CEO of Professional Science Editing for Scientists @ prosciediting.com