Optical depth (astrophysics)
Optical depth in astrophysics refers to a specific level of transparency. Optical depth and actual depth, and respectively, can vary widely depending on the absorptivity of the astrophysical environment. Indeed, is able to show the relationship between these two quantities and can lead to a greater understanding of the structure inside a star.
The assumption here is that either the extinction coefficient or the column number density N is known. These can generally be calculated from other equations if a fair amount of information is known about the chemical makeup of the star. From the definition, it is also clear that large optical depths correspond to higher rate of obscuration. Optical depth can therefore be though of as the opacity of a medium.
The extinction coefficient can be calculated using the transfer equation. In most astrophysical problems, this is exceptionally difficult to solve since solving the corresponding equations requires the incident radiation as well as the radiation leaving the star. These values are usually theoretical.
In some cases the Beer-Lambert Law can be useful in finding .
where is the refractive index, and is the wavelength of the incident light before being absorbed or scattered. It is important to note that the Beer-Lambert Law is only appropriate when the absorption occurs at a specific wavelength, . For a gray atmosphere, for instance, it is most appropriate to use the Eddington Approximation.
Therefore, is simply a constant that depends on the physical distance from the outside of a star. To find at a particular depth z, the above equation may be used with and integration from to .
The Eddington Approximation and the Depth of the Photosphere
Devised by Sir Arthur Eddington the approximation takes into account the fact that produces a "gray" absorption in the atmosphere of a star, that is, it is independent of any specific wavelength and absorbs along the entire electromagnetic spectrum. In that case,
where is the effective temperature at that depth and is the optical depth.
This illustrates not only that the observable temperature and actual temperature at a certain physical depth of a star vary, but that the optical depth plays a crucial role in understanding the stellar structure. It also serves to demonstrate that the depth of the photosphere of a star is highly dependent upon the absorptivity of its environment. The photosphere extends down to a point where is about 2/3, which corresponds to a state where a photon would experience, in general, less than 1 scattering before leaving the star.
The above equation can be rewritten in terms of in the following way:
Which is useful, for example, when is not known but is.