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Published equation contexts

Z≡1−X−YZ \equiv 1 - X - Y

Why this formula appears here

Zoom out from individual nuclei to the gas that forms whole generations of stars, and the genealogy becomes explicit rather than metaphorical. Astronomers describe the abundance of everything heavier than helium in a star or a cloud of gas with a single number, metallicity, defined through the mass fractions of hydrogen ( X ), helium ( Y ) and “metals” ( Z ): Z≡1−X−YZ \equiv 1 - X - Y. A gas cloud’s metallicity is, quite literally, an inherited character: it is the accumulated, largely unerased record of every previous generation of stars that lived, burned and returned processed material to the interstellar medium before that cloud collapsed to form new stars. The first stars, Population III,…

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ZZ

Symbol Z

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XX

Symbol X

X is a part of this expression. Its role is fixed by the surrounding article and by the operations shown in the formula.

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YY

Symbol Y

Y is a part of this expression. Its role is fixed by the surrounding article and by the operations shown in the formula.

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Published contexts (1)

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Z≡1−X−YZ \equiv 1 - X - Y

Equation 8 · Evolutionary Nuclear Physics

Nucleosynthesis Is Descent With Modification

This mathematical expression combines the displayed quantities; its precise role follows from the surrounding article text.

Zoom out from individual nuclei to the gas that forms whole generations of stars, and the genealogy becomes explicit rather than metaphorical. Astronomers describe the abundance of everything heavier than helium in a star or a cloud of gas with a single number, metallicity, defined through the mass fractions of hydrogen ( X ), helium ( Y ) and “metals” ( Z ): Z≡1−X−YZ \equiv 1 - X - Y. A gas cloud’s metallicity is, quite literally, an inherited character: it is the accumulated, largely unerased record of every previous generation of stars that lived, burned and returned processed material to the interstellar medium before that cloud collapsed to form new stars. The first stars, Population III,…

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