OFBAGKM.
OBAGFKM.
OBAFGKM.
ABFGKMO.
BAGFKMO.
Surface temperature on the horizontal axis and luminosity on the vertical axis
Mass on the horizontal axis and luminosity on the vertical axis
Surface temperature on the horizontal axis and radius on the vertical axis
Mass on the horizontal axis and stellar age on the vertical axis
Interior temperature on the horizontal axis and mass on the vertical axis
Watts
Joules
Newtons
Kilograms
Watts per second
Luminosity = apparent brightness / 4Ï€ x (distance)^2
Apparent brightness = luminosity / 4Ï€ x (distance)^2
Apparent brightness = luminosity x 4Ï€ x (distance)^2
Distance = luminosity / 4Ï€ x (apparent brightness)^2
Apparent brightness of the star in our sky.
Surface temperature of the star.
Lifetime of the star.
Total amount of light that the star will radiate over its entire lifetime.
Total amount of light that the star radiates each second.
Upper right
Lower right
Upper left
Lower left
Location where they are formed
Time they are formed
Luminosity they are formed with
Mass they are formed with
Color they are formed with
Upper right
Lower right
Upper left
Lower left
10 light-years.
10 parsecs.
0.1 light-year.
0.1 parsec.
Impossible to determine.
Upper right
Lower right
Upper left
Lower left
Mass.
Surface temperature.
Luminosity.
Core temperature.
Radius.
Visual binary
Eclipsing binary
Spectroscopic binary
Double star
None of the above
I
II
III
IV
V
Upper right
Lower right
Upper left
Lower left
All stars in the cluster are approximately the same color.
All stars in the cluster are approximately the same age.
All stars in the cluster have approximately the same mass.
All stars in the cluster will evolve similarly.
There is an approximately equal number of all types of stars in the cluster.
Low-mass stars are cooler and less luminous than high-mass stars.
Low-mass stars are hotter and more luminous than high-mass stars.
Low-mass stars are cooler but more luminous than high-mass stars.
Low-mass stars are hotter but less luminous than high-mass stars.
Low-mass stars have the same temperature and luminosity as high-mass stars.
Main sequence fitting.
Main sequence turnoff.
Pulsating variable stars.
Spectroscopic binaries.
Cluster ages can be determined from A) main sequence fitting. B) main sequence turnoff. C) pulsating variable stars. D) spectroscopic binaries. E) visual binaries.
Is decreased by a factor of four, and the apparent brightness is decreased by a factor of four.
Is decreased by a factor of two, and the apparent brightness is decreased by a factor of two.
Remains the same, but the apparent brightness is decreased by a factor of two.
Remains the same, but the apparent brightness is decreased by a factor of four.
Is decreased by a factor of four, but the apparent brightness remains the same.
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