Wrong Explanations for the Luminosity of Main-Sequence Stars

[TEFLing]

...

Also, if you use diffusion physics to get L, you never need L ~ M² / R³ Tⁿ, you can just use L ~ R⁴ T⁴ / M from diffusion with constant opacity (or modify that for some other opacity like Kramers, but it won't be more accurate), and T ~ M/R from VT, and get L without even saying whether fusion is happening or not...

M² / R³ Tⁿ ~ L ~ R⁴ T⁴ / M

M³ Tⁿ ~ R⁷ T⁴ ~ R³ M⁴

Tⁿ ~ R³ M ~ R⁴ T

T^n-1 ~ R⁴ ~ M/R ~ M/T^(n-1)/4

T^5(n-1)/4 ~ M ~ R⁵

L ~ M^2/5 M^16/5(n-1)

n=4
-----
L ~ M^1.5

Seems like the two equations for L are not compatible...(??)

 

[TEFLing]

I want to ask about the VT...

Isn't the VT based on the IGL and an assumption of HSE?

For, the VT is consistent with the one zone scaling relation form of the HSE equation

dP/dr = -rho g

P/R ~ M² / R⁵

rho T ~ rho g R

T ~ M/RBUT what if pressure support derives from RADIATION pressure, not gas pressure??

Wouldn't wht

dP/dr = -rho g

P/R ~ M² / R⁵

T⁴ ~ M² / R⁴

T ~ sqrt(M) / R

 

[Ken G]

T^n-1 ~ R⁴ ~ M/R ~ M/T^(n-1)/4

Wasn't there a problem in the middle there?

 

[Ken G]

I want to ask about the VT...

Isn't the VT based on the IGL and an assumption of HSE?

Yes exactly.

BUT what if pressure support derives from RADIATION pressure, not gas pressure??

Then you need a different form for the VT, but it's only an issue for the highest mass stars.

T⁴ ~ M² / R⁴

T ~ sqrt(M) / R

Radiation P is not T⁴, it is ~ T⁴/R³. You should ultimately find the Eddington limit: L ~ M, if you take constant opacity.

 

[TEFLing]

If we have scaling relations...

L ~ R² T⁴
L ~ M² Tⁿ / R³
T ~ M/R or M^1/2 / R

Gas support
==========
R² T⁴ ~ (RT)² Tⁿ / R³ ~ Tⁿ⁺² / R

R³ ~ T^n-2

M³ ~ Tⁿ⁺¹

L ~ R² T⁴ ~ T^2(n-2)/3 M^12/(n+1) ~ M^2(n-2)/(n+1) M^12/(n+1) ~ M^(2n+8)/(n+1)

L ~ M^3.2 (n=4)
Radiation support
===============
R² T⁴ ~ (RT)⁴ Tⁿ / R³

R ~ Tⁿ

M^1/2 ~ Tⁿ⁺¹

L ~ R² T⁴ ~ T²ⁿ M^2/(n+1) ~ M^n/(n+1) M^2/(n+1) ~ M^(n+2)/(n+1)

L ~ M^1.1 (n=18)Isn't this qualitatively correct? Doesn't L ~ M for high mass stars?

 

[TEFLing]

Take x2...
========

M² / R³ Tⁿ ~ L ~ R⁴ T⁴ / M

M³ Tⁿ ~ R⁷ T⁴ ~ R³ M⁴

Tⁿ ~ R³ M ~ R⁴ T

T^n-1 ~ R⁴

T ~ R^4/(n-1) ~ M/R

M ~ R^(n+3)/(n-1)

R ~ M^(n-1)/(n+3)

T ~ M^4/(n+3) L ~ R² T⁴ ~ M^{(2n+14)/(n+3)}

n=4
L ~ M^22/7

 

[Ken G]

Radiation support
===============
R² T⁴ ~ (RT)⁴ Tⁿ / R³

R ~ Tⁿ

M^1/2 ~ Tⁿ⁺¹

L ~ R² T⁴ ~ T²ⁿ M^2/(n+1) ~ M^n/(n+1) M^2/(n+1) ~ M^(n+2)/(n+1)

L ~ M^1.1 (n=18)Isn't this qualitatively correct? Doesn't L ~ M for high mass stars?

It is qualitatively correct, but it's kind of a coincidence. What actually happens is L ~ M exactly, if we use constant opacity, and the value of n makes no difference at all. The flaw in this analysis is that it assumes the core T and the surface T are either the same, or at least proportional, and there's no physical basis for that assumption. All the same, since it works out to be approximately true that they are proportional, you can get away with asserting it in the derivation. But doing so puts the cart before the horse-- we know L ~ M for other reasons (the Eddington limit), so your scaling analysis should actually be used to derive the ratio of surface T to interior T. When you find that the two are approximately proportional, you have demonstrated something important, but it's not the same thing being demonstrated as if you just assume that from the start.

 

[Ken G]

Take x2...
========

M² / R³ Tⁿ ~ L ~ R⁴ T⁴ / M

M³ Tⁿ ~ R⁷ T⁴ ~ R³ M⁴

Tⁿ ~ R³ M ~ R⁴ T

T^n-1 ~ R⁴

T ~ R^4/(n-1) ~ M/R

M ~ R^(n+3)/(n-1)

R ~ M^(n-1)/(n+3)

T ~ M^4/(n+3)L ~ R² T⁴ ~ M^{(2n+14)/(n+3)}

n=4
L ~ M^22/7

Yes, that's bang on. So we see we have some subjective freedom as to how we will derive L. We can take an n for nuclear burning, even though that will limit our range of applicability (p-p fusion doesn't dominate past a solar mass), and give exactly the analysis you have. You get a slightly complicated power in the mass-luminosity relation, but it is quite useful all the same, and works fine. Alternatively, we can ignore any need to assert an n for fusion, and just say that fusion induces a thermostatic effect that regulates T to be something like 20 million K. Unfortunately this will not be at all exact, but we do get a very bare bones kind of derivation that gives L ~ M³. A simpler power, simpler physics, but not more justifiable-- just a different set of things to idealize. So it's a subjective choice at this point.

 

[TEFLing]

http://www.physics.rutgers.edu/~pryor/ph442/lecture12.pdf

I found the above link for the index of refraction of a plasma...

In slide 1 I think they mean to say n is IMAGINARY at low frequencies, not negative

I think at the high temperatures inside stars, n~1 is a very accurate approximation

 

[TEFLing]

Yes, that's bang on. So we see we have some subjective freedom as to how we will derive L. We can take an n for nuclear burning, even though that will limit our range of applicability (p-p fusion doesn't dominate past a solar mass), and give exactly the analysis you have. You get a slightly complicated power in the mass-luminosity relation, but it is quite useful all the same, and works fine. Alternatively, we can ignore any need to assert an n for fusion, and just say that fusion induces a thermostatic effect that regulates T to be something like 20 million K. Unfortunately this will not be at all exact, but we do get a very bare bones kind of derivation that gives L ~ M³. A simpler power, simpler physics, but not more justifiable-- just a different set of things to idealize. So it's a subjective choice at this point.

WOW

I think I almost understand what you are saying

Roughly speaking, we start with a diffusion equation for the starlight, which is time invariant, d/dt -> 0

=> constant Laplacian double derivative on the other side...

Implying a constant heat flow

L ~ c l d/dr(4 pi r2 T4)

Where l~1/(rho sigma) is a mean free path measure

So the scaling relation simplification is

L ~ L / ( rho sigma T )

Rho sigma R ~ constant

Which says that if a star becomes more opaque per particle, the column density of particles must decrease to let the same light luminosity out through the plasma to the surface

Assuming ES is dominant, sigma ~ constant, and rho R must be constant too

==============
Using FF opacity

Sigma ~ rho T^-3.5

Rho sigma R ~ rho^2 T^-3.5 R ~ 1

M^2/R^5 ~ T^3.5

-----------------------
Using VT , RT ~ M

M^2 ~ R^1.5 M^3.5

1 ~ (RM)^1.5

M ~ 1/R

(??)-----------------------
Using VT , RT ~ sqrt(M)

M^2/R^5 ~ T^3.5

M^2 ~ R^1.5 M^1.75

M^.25 ~ R^1.5

M ~ R^6

M^2/R^5 ~ T^3.5

M^7/6 ~ T^7/2

M ~ T^3

L ~ R2T4 ~ M^.333 M^1.333 ~ M^5/3

 

[Ken G]

Implying a constant heat flow

L ~ c l d/dr(4 pi r2 T4)

Where l~1/(rho sigma) is a mean free path measure

Yes, this is correct.

So the scaling relation simplification is

L ~ L / ( rho sigma T )

Rho sigma R ~ constant

I wasn't sure what you were getting at here. We both get L ~ d/dtau(r² T⁴), where dtau = sigma*rho*dr is the optical depth across dr, and r² T⁴ is like the radiative energy per shell of unit radial length. This is like setting dtau=1 and using the shells you were talking about above. Where I would go with that is just insert the characteristic proportionality tau ~ M/R² for constant sigma (for simplicity, or as a benchmark for comparison), yielding L ~ (RT)⁴/M. So that's all we can get from radiative diffusion, and if we take M as given, then the L depends only on RT if sigma is constant. Then the VT shows that RT is also constrained by M, since RT ~ M. Thus L depends only on M. You can use different opacity laws, which will introduce some independent dependence on R and T, which will in turn bring in the fusion physics (and the power n) because T will now matter, but if constant-sigma dominates, that won't occur, and if n is large (as for CNO cycle), then the T physics is highly thermostatic and it also won't matter much how the fusion changes as M changes, i.e., the explicit value of n won't matter if n is large. But you are right that for M ~ 0.5 solar, we have p-p fusion with n = 4, and it only goes up to about n = 5 for solar M, so those values of n are small enough that some fusion physics will end up showing up in L, as will some Kramers opacity effects. You only get the super-simple result L ~ M³ if you ignore those details, but then we are also ignoring convection and radiative forces, so we are already going to be stuck with some pretty rough results.

You are also looking at the scaling laws for R(M), so they will start with R ~ M/T and have to use some fusion physics to get T, but for higher mass stars, again T will be fairly thermostatic, around 20 MK to 30 MK, so you won't do too badly with R ~ M. For lower M stars, the lower n of p-p fusion makes R(M) drop less rapidly as M drops, and convection also becomes more of an issue, so again it's a matter of what subjective tradeoffs you want to make in your idealizations.

I wouldn't try to get surface T until the end-- once I have a handle on both L and R, I would then say the surface T is ~ L^1/4/R^1/2. The surface T rarely has much input into either L or R, so that last formula is not very useful as an input to either the L or the R determination. However, you have seen some nice scaling relations about the ratio of surface to core T.

 

[TEFLing]

Yes, this is correct.
I wasn't sure what you were getting at here. We both get L ~ d/dtau(r² T⁴), where dtau = sigma*rho*dr is the optical depth across dr, and r² T⁴ is like the radiative energy per shell of unit radial length. This is like setting dtau=1 and using the shells you were talking about above. Where I would go with that is just insert the characteristic proportionality tau ~ M/R² for constant sigma (for simplicity, or as a benchmark for comparison), yielding L ~ (RT)⁴/M. So that's all we can get from radiative diffusion, and if we take M as given, then the L depends only on RT if sigma is constant. Then the VT shows that RT is also constrained by M, since RT ~ M. Thus L depends only on M. You can use different opacity laws, which will introduce some independent dependence on R and T, which will in turn bring in the fusion physics (and the power n) because T will now matter, but if constant-sigma dominates, that won't occur, and if n is large (as for CNO cycle), then the T physics is highly thermostatic and it also won't matter much how the fusion changes as M changes, i.e., the explicit value of n won't matter if n is large. But you are right that for M ~ 0.5 solar, we have p-p fusion with n = 4, and it only goes up to about n = 5 for solar M, so those values of n are small enough that some fusion physics will end up showing up in L, as will some Kramers opacity effects. You only get the super-simple result L ~ M³ if you ignore those details, but then we are also ignoring convection and radiative forces, so we are already going to be stuck with some pretty rough results.

You are also looking at the scaling laws for R(M), so they will start with R ~ M/T and have to use some fusion physics to get T, but for higher mass stars, again T will be fairly thermostatic, around 20 MK to 30 MK, so you won't do too badly with R ~ M. For lower M stars, the lower n of p-p fusion makes R(M) drop less rapidly as M drops, and convection also becomes more of an issue, so again it's a matter of what subjective tradeoffs you want to make in your idealizations.

I wouldn't try to get surface T until the end-- once I have a handle on both L and R, I would then say the surface T is ~ L^1/4/R^1/2. The surface T rarely has much input into either L or R, so that last formula is not very useful as an input to either the L or the R determination. However, you have seen some nice scaling relations about the ratio of surface to core T.

Conceptually I think you have an equation like

L ~ d/dtau ( r2 T4) ~ ( Lcore - Lsurfsce)/( M/R2)

I think you can then use scaling relations like

Lcore ~ M rho T^n

And ignore Lsurface on the RHS since it's smaller than Lcore

Seemingly you're saying that the L seen at the surface is the original core luminosity stepped down like a voltage transformer , by the number of MFP i.e. optical depth

Assuming constant opacity, and using n=4,18 and RT ~ M, sqrt(M)...

You seem to get

L ~ M3 for low mass stars
L ~ M2 for intermediate mass stars
L ~ M for high mass stars

 

[Ken G]

I get L ~ M³ for all stars, independent of n, if I assume gas pressure dominates over radiation pressure, ideal gas T, ignore convection, and assume fixed opacity. I don't even need to say if fusion is even happening to get this, indeed look at the tracks of pre-main-sequence stars in an H-R diagram to see just how unnecessary it is to say if fusion is happening to get L.

If we instead use radiation pressure, instead of gas pressure, we get the Eddington limit value for L, which obeys L ~ M for constant opacity and no convection, and doesn't need to know anything about T or n. You'd actually get a lot of convection, but it might only carry some of the L, so the L ~ M is probably still not too bad.