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The new D-value for 160 °C given the z-value is 0.45 minutes. This means that each 10 °C (18 °F) increase in temperature will reduce our D-value by 1 log. Conversely, a 10 °C (18 °F) decrease in temperature will increase our D-value by 1 log. So, the D-value for a temperature of 140 °C would be 45 minutes.
The effective temperature of the Sun (5778 kelvins) is the temperature a black body of the same size must have to yield the same total emissive power.. The effective temperature of a star is the temperature of a black body with the same luminosity per surface area (F Bol) as the star and is defined according to the Stefan–Boltzmann law F Bol = σT eff 4.
Gas mark 1 is 275 degrees Fahrenheit (135 degrees Celsius). [citation needed]Oven temperatures increase by 25 °F (14 °C) for each gas mark step. Above Gas Mark 1, the scale markings increase by one for each step.
where G is the gravitational constant, M is the mass of the star, R is the radius of the star, and L is the star's luminosity. As an example, the Sun 's thermal time scale is approximately 15.7 million years.
Thus, from the Stefan–Boltzmann law, the luminosity is related to the surface temperature T S, and through it to the color of the star, by = where σ B is Stefan–Boltzmann constant, 5.67 × 10 −8 W m −2 K −4. The luminosity is equal to the total energy produced by the star per unit time.
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In astronomy, the color index is a simple numerical expression that determines the color of an object, which in the case of a star gives its temperature. The lower the color index, the more blue (or hotter) the object is. Conversely, the larger the color index, the more red (or cooler) the object is.