I Why is the density of photons in the Eddington Limit derived this way?

AI Thread Summary
The discussion centers on the derivation of the Eddington limit, specifically the formula for photon density in an accretion flow. The density of photons is expressed as n_ph = L_ν / (4πr²chν), which raises questions about its formulation. It is clarified that while L_ν represents energy flux, dividing by hν converts it to photon flux, and further division by c transforms it to a density of particles per volume. An alternative perspective suggests that understanding the Eddington limit in terms of momentum flux per area is more straightforward than focusing solely on photon density. The conversation concludes with a query about the necessity of restating the Eddington limit in terms of photons.
Aleolomorfo
Messages
70
Reaction score
4
I am studyng accretion process on "Astrophysics in a nutshell" by Dan Maoz and I have some doubts about the derivation of the formula for the eddington limit. I understand what the edding limit is. The accretion rate cannot be arbitrarly large. The starting point is to consider an electron at a radius ##r## in an ionized gas that is taking part in an accretion flow towards some compact object. The accretion flow produces a luminosity per frequency interval ##L_\nu##, and therefore the density of photons with energy ##h\nu## at ##r## is:
$$n_{ph}=\frac{L_\nu}{4\pi r^2 ch\nu}$$
I do not understand why the density of photons is written in this way. I see that it is dimensionally correct but I do not see the reason.
##\frac{L_\nu}{4\pi r^2}## is the flux of photons with frequency ##\nu## but I do not understand why it is divided by ##ch\nu##.
 
Astronomy news on Phys.org
L_{\nu} is not the flux of photons, it is the flux of energy. So you have to divide by the energy per photon to get the flux of photons.
 
  • Like
Likes stefan r
Yes, you first have to divide by the energy per photon, h*nu, to get it into a number flux (and I believe you mean flux per area), but then you also have to divide by the particle speed to get it into a density of particles per volume. You'd have to do the same thing with a flux of bullets. If you still don't see it, it might help to take the c up onto the left side of the equation, and think about what a number density times a speed is.

However, I would also point out that the easiest way to understand the Eddington limit is to think in terms of the momentum flux per area, not the photon flux and not the photon density. This is because to get the radiative force per gram, you simply take the momentum flux per area, and multiply by the cross section per gram. That's the simplest way to see what is going on.
 
  • Like
Likes Aleolomorfo
Aleolomorfo said:
therefore the density of photons with energy hνhνh\nu at rrr is:
Is there any special point in restating the Eddington limit in terms of photons?
 
Is a homemade radio telescope realistic? There seems to be a confluence of multiple technologies that makes the situation better than when I was a wee lad: software-defined radio (SDR), the easy availability of satellite dishes, surveillance drives, and fast CPUs. Let's take a step back - it is trivial to see the sun in radio. An old analog TV, a set of "rabbit ears" antenna, and you're good to go. Point the antenna at the sun (i.e. the ears are perpendicular to it) and there is...
3I/ATLAS, also known as C/2025 N1 (ATLAS) and formerly designated as A11pl3Z, is an iinterstellar comet. It was discovered by the Asteroid Terrestrial-impact Last Alert System (ATLAS) station at Río Hurtado, Chile on 1 July 2025. Note: it was mentioned (as A11pl3Z) by DaveE in a new member's introductory thread. https://www.physicsforums.com/threads/brian-cox-lead-me-here.1081670/post-7274146 https://earthsky.org/space/new-interstellar-object-candidate-heading-toward-the-sun-a11pl3z/ One...
Back
Top