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Star 306 consists of a pair of stars which eclipse each other.
They are so close together that they are pulled out of a spherical
shape by tidal forces. The light curve between eclipses is not flat,
because of the changing aspect of the distorted stars as they move in
their orbits. |
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Star 315 is a suspected delta scuti pulsating variable. Light
curves of this type of variable are almost exact reflections of the
radial-velocity curves. Typical periods range from .01 to .2 days and
amplitudes range from .003 to .9 mag.
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Star 875 is a suspected delta cepheid pulsating variable. Delta
cepheids are fairly young stars that have left the main sequence and
evolved into the instability strip of the H-R diagram. They display a
certain relationship between the shapes of their light curves and their
periods.
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Star 887 is a suspected beta cepheid pulsating variable. The
curves of these variables are similar in shape to average
radial-velocity curves, but lag in phase by a quarter of the period so
that maximum brightness corresponds to maximum contraction.
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Star 1025 is another detached binary, but with a much smaller
(4%) primary eclipse. The very small eclipse depth may indicate that
one star is only about 0.2 times as large as the other, or that the
orbital plane is tilted to our line of sight, so that grazing eclipses
occur. The eclipse depth in this case is about 4 times as large as one
would expect for a Jupiter-sized planet.
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