Show This means that if you double the temperature of an star, it will radiate 2 x 2 x 2 x 2 = 16 times as much energy per square unit of area, and also in total if its surface area doesn't change.
Something strange is happening here! The Sun has a higher surface temperature, so it must radiate more energy per unit surface area than Ori. In spite of this, Ori has a far greater luminosity than the Sun! There is only one way that Ori could radiate more total energy – it must have a larger total surface area.
The energy, E, emitted by a star (equivalent to the luminosity, L) is proportional to the square of the radius, R, and the fourth power of the temperature, T. We can express these quantities as a ratio between the properties of two stars:
By making one of the two stars the Sun, we can express the properties of any star in solar units.
Thanks to Mike Bolte (UC Santa Cruz) for the base contents of this slide. What is the temperature of a star directly related to?The effective temperature is directly related to the color of the star: the higher the temperature, the bluer the light emitted by the star. The effective temperature is one of the two parameters, with the stellar luminosity, used to build the classical HR diagram that permits astronomers to classify stars.
What factor affects the temperature of a star?The surface temperature is determined by the luminosity and radius. The luminosity is governed by the central temperature. An increase in mass, increases the central temperature and greatly increases the luminosity. The radius also increases, but not by enough to compensate, so the surface temperature also rises.
What determines the temperature of a star?A star's surface temperature can be determined from its spectrum. The Hertzsprung-Russell diagram sorts stars by luminosity and temperature. Most stars are on the main sequence of the Hertzsprung-Russell diagram.
What property of a star can most directly be used to determine its temperature?Measuring the strength of the hydrogen absorption lines is usually the first step for determining a star's temperature. If the star is too hot or too cold, the hydrogen lines will be weak. To produce strong, dark hydrogen lines, the star's temperature must be within a certain range.
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