Calculating the stars6/2/2023 ![]() ![]() Both of these conditions are hard to satisfy in practice: stars are in general not blackbodies, though their effective temperatures - which is usually what is quoted, are defined as the temperature of a blackbody with the same radius and luminosity of the star. This method could be used to estimate the temperatures of objects that have spectra which closely approximate blackbodies and for which flux-calibrated spectra are available that properly sample the peak. ![]() Gerald has talked about the blackbody spectrum - indeed the wavelength of the peak of a blackbody spectrum is inversely dependent of temperature through Wien's law. We put the star back into the rest-frame before analysing its spectrum. It is a reasonably simple procedure to correct for the line of sight velocity of a star, because the redshift (or blueshift) applies to all wavelengths equally and we can simply shift the wavelength axis to account for this. Stars do of course have line of sight velocities which give their spectrum a redshift (or blueshift). When we talk about measuring the temperature of a star, the only stars we can actually resolve and measure are in the local universe they do not have appreciable redshifts and so this is rarely of any concern. ![]() This question is very broad - there are very many techniques for estimating temperatures, so I will stick to a few principles and examples. ![]()
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