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The temperature of a star is determined for it's colour spectrum. The hotter the star the more the spectrum is towards blue where as a cooler star has a spectrum closer to red.
For nearby stars, the parallax method is used.
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Iron
Elements are identified based on their absorption spectra. Every element absorbs a unique set of frequencies when light passes through it. Scientists can determine which elements are present based on which portions of the star's light are absorbed.
What elements the star is made of.
using a telescope to determine the coordinates of a star
Our Sun is about 70% Hydrogen and 28% Helium by mass, with traces of heavier elements. Other stars can be a little different, but with a spectrometer, scientists are able to determine the elements that are present in any star.
Hydrogen and helium are the most abundant elements in a star.
By the star's spectrum.
They use a tool called a SPECTROSCOPE.
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They can do so by examining the light from the star. Doppler shift can indicate this
Elements that exist in the start
Our Sun is about 70% Hydrogen and 28% Helium by mass, with traces of heavier elements. Other stars can be a little different, but with a spectrometer, scientists are able to determine the elements that are present in any star.
Atoms in a star's corona are subjected to extremely high levels of energy from the photosphere. This energy excites electrons in the atoms, and causes the electrons to jump up to a higher energy state. When the electrons fall back to their rest state, they emit photons at a very specific set of wavelengths unique to each element. By examining the wavelengths of light coming from a specific star (in a process called astronomical spectroscopy) astronomers are able to decipher with complete certainty which elements are present in that star. . For example, hydrogen emissions are known to occur at 410.2nm (violet), 434.1nm (violet), 486.1nm (blue-green), and 656.3nm (red). When a star is seen to emit a combination of those wavelengths, astronomers can be certain hydrogen is present in the star under observation. . See the related link below for more information on emission spectra.