The mass-luminosity relation applies to both white dwarfs and main-sequence stars as both trace linear lines on the H-R diagram.
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Q145: When we see a binary system producing
Q146: White dwarfs are dense, cool, and dim.
Q147: Stars of spectra type K have strong
Q148: The more massive star in a binary
Q149: The luminosity of a star is the
Q151: The larger variation in brightness of a
Q152: In an eclipsing binary, the orbits are
Q153: An M star is hotter than an
Q154: On the H-R diagram, lines of constant
Q155: The larger variation in brightness in an
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