On a logarithmic scale for luminosity, it is quite close to a negative linear relationship.
The scatter plot of the relationship between a star's temperature and luminosity is represented by the Hertzsprung-Russell diagram. In a standard H-R diagram the horizontal axis shows the [surface] temperature, increasing from right to left, while the vertical axis shows luminosity increasing from bottom to top. When both axis are on a logarithmic scale, the main sequence stars from a diagonal belt stretching from top right (very hot and very luminous) to bottom left (not so hot and not so luminous).
On such a diagram, those stars lie on a curve called the "main sequence". It is not a simple relationship - for example, it isn't a straight line on the diagram. Therefore, it isn't easy to describe in words. It's best if you look up "Main sequence", for example on the Wikipedia, and look at the corresponding diagram.
There is no simple relation. The color does not depend only on the mass. The same star can change color, without a significant change in mass. For example, our Sun is currently yellow; in a few billion years, it is expected to get much larger, becoming a red giant. However, if we limit the sample of stars to those on the "main sequence" of the "HR diagram", there is something of a relation between mass and color. The most massive stars are blue or white. They are also hottest and most luminous. The least massive are the red dwarf stars, which are relatively cool and dim. Our Sun, which is a "main sequence" star at present, is somewhere in between those extremes. (There is a strong relationship between mass and luminosity for main sequence stars. The HR diagram, of course, shows there is a relationship between luminosity and color for the main sequence stars.)
Between 11,000 and 25,000 Kelvin, or about 40,000 times the luminosity of the sun.
The life cycle of a star is determined primarily by its mass. The hotter a star the bluer its color. The difference between apparent brightness and luminosity is that luminosity is a good indicator of the energy output of a star.
as surface temperature increases, luminosity increases
No. Main sequence stars are simply stars that are fusing hydrogen into helium and have a specific relationship between color and luminosity. They range from red dwarfs to large O-type main sequence stars.
The scatter plot of the relationship between a star's temperature and luminosity is represented by the Hertzsprung-Russell diagram. In a standard H-R diagram the horizontal axis shows the [surface] temperature, increasing from right to left, while the vertical axis shows luminosity increasing from bottom to top. When both axis are on a logarithmic scale, the main sequence stars from a diagonal belt stretching from top right (very hot and very luminous) to bottom left (not so hot and not so luminous).
Cepheids have a certain relationship between their period, and their absolute luminosity. Thus, their absolute luminosity can be determined. Comparing this with their apparent luminosity allows us to calculate their distance.Cepheids have a certain relationship between their period, and their absolute luminosity. Thus, their absolute luminosity can be determined. Comparing this with their apparent luminosity allows us to calculate their distance.Cepheids have a certain relationship between their period, and their absolute luminosity. Thus, their absolute luminosity can be determined. Comparing this with their apparent luminosity allows us to calculate their distance.Cepheids have a certain relationship between their period, and their absolute luminosity. Thus, their absolute luminosity can be determined. Comparing this with their apparent luminosity allows us to calculate their distance.
The star that is hotter will have a higher luminosity.
The star that is hotter will have a higher luminosity.
On such a diagram, those stars lie on a curve called the "main sequence". It is not a simple relationship - for example, it isn't a straight line on the diagram. Therefore, it isn't easy to describe in words. It's best if you look up "Main sequence", for example on the Wikipedia, and look at the corresponding diagram.
There is no simple relation. The color does not depend only on the mass. The same star can change color, without a significant change in mass. For example, our Sun is currently yellow; in a few billion years, it is expected to get much larger, becoming a red giant. However, if we limit the sample of stars to those on the "main sequence" of the "HR diagram", there is something of a relation between mass and color. The most massive stars are blue or white. They are also hottest and most luminous. The least massive are the red dwarf stars, which are relatively cool and dim. Our Sun, which is a "main sequence" star at present, is somewhere in between those extremes. (There is a strong relationship between mass and luminosity for main sequence stars. The HR diagram, of course, shows there is a relationship between luminosity and color for the main sequence stars.)
Their distance away from you and their intrinsic luminosity.
The difference between apparent brightness and luminosity is that apparent brightness means that a star may appear to be bright, but only looks bright because of the relatively closeness a star is to earth. Luminosity is used by astronomers and refers to the power output of a star. Apparent Brightness means a star may appear to be very bright but only look that way because it is relatively close to Earth. Luminosity just refers to the power output of a star.
The difference between apparent brightness and luminosity is that apparent brightness means that a star may appear to be bright, but only looks bright because of the relatively closeness a star is to earth. Luminosity is used by astronomers and refers to the power output of a star. Apparent Brightness means a star may appear to be very bright but only look that way because it is relatively close to Earth. Luminosity just refers to the power output of a star.
Between 11,000 and 25,000 Kelvin, or about 40,000 times the luminosity of the sun.