Radiative transfer Definition and 11 Threads

\begin{equation} \chi = n \sigma \end{equation} Where Chi is the Opacity, n is the number density of absorbers (constant), and $\sigma$ is the cross section(given). We define the optical depth is just the number of photon mean-free paths in a given physical step, i.e. if we consider a...

Hi, I'm currently working on thermal radiation modelling in my PhD studies, and one thing that's under work is a cylindrical symmetric thermal radiation solver code. The idea is to solve the thermal radiation field in an absorbing medium between concentric cylinders as an essentially 1D problem...

Hey guys, I'm really stuck right now 1. Homework Statement Habitable exoplanet: Now we will include a convective heat flux (H), with H being proportional to the difference between the atmospheric and ground surface temperature, $$H=c_p(T_a-T_p)$$ with c = 1.2 Wm−2K−1. Calculate the temperature...

Homework Statement Within a certain material, an EM wave with = 1 mm is attenuated to 10% of its original intensity after propagating 10 cm. Determine the imaginary part of the index of refraction ni Homework Equations 3. The Attempt at a Solution [/B] so...

for the following formulation of the RTE, Why do we reformulate in terms of μ = cosθ?

Re: the absorption & re-emission of long-wave radiation in the Earth's atmosphere. I thought it all made sense until I was trying to work out how to explain it better to others! So the Beer-Lambert equation describes the absorption at a given wavelength as exp(-k.z) where k is a constant...

Hi, I'm new to the technical aspects of astronomy and I'm having trouble quantifying what the definitions of some of these terms are. I can find equations that relate most of them, but I'm not sure how to use any of them. The terms are specific intensity, flux, flux density, and monochromatic...

I'm trying to model radiation losses from a flat surface facing the sky at night. If we ignore radiative absorption/emission in the atmosphere, the heat flux is the well-known Q=\epsilon\sigma(T_s^4-T_\infty^4) where we have the emissivity, the S-B constant, the temperature of the surface...

Homework Statement An optically thin cloud at temperature T radiates power P_{\nu} per unit volume. Find an expression for the cloud's brightness I_{\nu} as a function of distance from the centre of the cloud in the case where: (a) the cloud is a cube of side d (b) the cloud is a sphere...

Could someone please suggest a reference from where I could read up radiative transfer physics?