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A large body of evidence suggests that all members of this first class
of variable stars owe their variability to pulsation. The
pulsation theory was
first proposed as a possible explanation as early as 1879, was applied
to Cepheids in 1914, and was further developed by Arthur Eddington in
1917–18. Eddington found that if stars have roughly the same kind of
internal structure.
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