What is the formula for calculating the temperature of a star?

Answer 1

Well, sweetheart, to calculate the temperature of a star, you can use Wien's Law which states that the temperature is inversely proportional to the peak wavelength of its emitted radiation. Another way is to use the Stefan-Boltzmann Law, which relates a star's luminosity and surface area to its temperature. So just plug those numbers in and bam, you've got yourself a hot, steamy star temperature!

Answer 2

The formula for calculating the temperature of a star is Wien's Law, which is expressed as T = b / λ, where T is the temperature of the star, b is a constant value (approximately 2.898 x 10^-3 m*K), and λ is the peak wavelength of the star's emitted radiation.

Answer 3

Oh, what a delightful question, my friend! Calculating the temperature of a star is as beautiful as the colors on your canvas. You can find it using the Wien's Law equation, which involves the star's peak wavelength or frequency of light. Just remember to approach it with a gentle hand and a happy heart. Bob Ross believes you can do it, and so do I.

Answer 4

Oh, dude, calculating the temperature of a star is like trying to figure out how many snacks you can eat in one sitting - you gotta be careful not to overdo it! So, the formula for star temperature is called Wien's Law, and it's like this fancy pants equation involving the star's peak wavelength and temperature. Basically, just plug in the numbers, do some math, and boom, you've got yourself a star temperature hotter than a jalapeno on a summer day!

Answer 5

The temperature of a star can be calculated using Wien's Law, which relates the temperature of an object to the peak wavelength of its emitted radiation. The formula is:

T = b / λmax

Where: T = Temperature of the star in Kelvin b = Wien's displacement constant, approximately 2.898 x 10^-3 meters-Kelvin λmax = Wavelength at which the intensity of radiation emitted by the star is greatest, typically in meters

To determine the peak wavelength of emitted radiation, one can use the Stefan-Boltzmann Law to find the star's luminosity and its radius. Then, by studying the star's spectrum, one can identify the wavelength at which the emitted radiation is most intense.

This formula allows astronomers to estimate the temperatures of stars based on their observed spectra and intensities of emitted radiation at different wavelengths.