Recent content by Kayla Martin

Okay, so the question that I am curious about this for, specifically says "A supernova remnant has an angular diameter θ = 4.3 arcminutes and a flux at 100 MHz of F100 = 1.6×10−22 Jm−2s−1Hz−1. Assume that the emission is thermal." Does that help at all? I figured that to calculate the value of...

I tried $$\Omega = \pi(\frac{\theta}{2})^{\frac{1}{2}}$$

Is it anything to do with the equation being independent of mass etc.. of the star? or to do with the Pauli exclusion principle? Any help will be much appreciated.

Am I able to direct message you to ask you another question that relates to this part seeing as you seem to know what you're doing?

Equations I think may be relevant:

The only solution (for part a) I can think of is if we use the radiative transfer equation without S... i.e. $$\frac{I}{\tau}= I_0 e^{-\tau}$$ and then take the natural log of each side to get $$\tau= -\ln(\frac{I}{I_0})$$ but I don't know if I can just get rid of S like that?