<p>Yes, there's a major problem. You are trying to run a &quot;device&quot; that uses up <span class="math-container">$350L_\odot$</span> with a <span class="math-container">$1L_\odot$</span> power source. In fact it's worse than that because the grains cannot absorb more than a small fraction of the solar luminosity if they are concentrated into a torus. That cannot be an equilibrium situation.</p>
<p>Let's imagine the torus has a thickness of <span class="math-container">$0.1$</span> au. The surface area of the torus would be <span class="math-container">$1.4\times 10^{22}$</span> m<span class="math-container">$^2$</span>, which represents only  5% of the surface area around the Sun at 1 au.</p>
<p>Your <span class="math-container">$2\times 10^{36}$</span> grains, each of radius <span class="math-container">$5\times 10^{-6}$</span> present a cross-sectional area of <span class="math-container">$1.6\times 10^{26}$</span> m<span class="math-container">$^2$</span>, which is 500 times the available area at 1 au.</p>
<p>i.e. The assumption of no self-shadowing doesn't hold water; the torus would be optically thick; and the emitting area would be of order <span class="math-container">$10^4$</span> times lower.</p>

CC BY-SA 4.0
2023-03-05T10:05:02.463Z
2023-03-05T10:05:02.463Z
ProfRob
<p>I've been told to &quot;consider an Earth-mass of interplanetary grains (roughly spherical with a radius of a few microns) in a protoplanetary disk. Let the particles be in a torus with a cross-section of the Hill radius of the Earth, at a distance of <span class="math-container">$1 \text{ AU}$</span> from a <span class="math-container">$1M_\odot$</span> protostar.&quot;</p>
<p>With this in mind, I must estimate the thermal velocity and mean time between collisions for the grains, and then compute the luminosity of the protoplanetary disk (ignoring any self-shadowing).</p>
<p>I'm content with my answer for thermal velocity &amp; mean collision time, but the luminosity I get is:</p>
<p><span class="math-container">$L_\text{disk} = 1.36 \times 10^{29} \text{ W} \approx 350 ~L_\odot$</span>.</p>
<p>Now, given the dramatic size difference, I expected the disk to be more luminous than the Sun, but this struck me as excessive. <strong>I'm hoping someone could please let me know if my methods are sound.</strong></p>
<p>(Obviously I am not asking anyone to do my homework for me, but rather to see if any assumption I've made stands out as utterly ridiculous or something along those lines. I've included my calculations to better demonstrate my thought process.)</p>
<p>My strategy was to consider the grains as collection of blackbody radiators and sum up their individual luminosities to obtain the disk's luminosity. I can estimate the equilibrium temperature of a grain using an assumed value for its albedo, which I can then use to calculate the re-radiated luminosity of each individual grain. I know the mass of the grains from their size and assumed density. I know the overall mass of the disk, so I can readily obtain the number of grains by dividing it by the grain mass. Multiplying the number of grains by their individual luminosity thus gives me the overall luminosity, since I'm told I can ignore self-shadowing.</p>
<p>My assumptions/simplifications:</p>
<ul>
<li>the grains are spherical and of radius <span class="math-container">$r_g = 5 \mu\text{m}$</span></li>
<li>the grains are composed of 'earthium' and therefore have the modern Earth's bulk density <span class="math-container">$\rho_g = \rho_\oplus = 5500 \text{ kg/m}^3$</span></li>
<li>the grains have a uniform temperature <span class="math-container">$T_g$</span>, which is to say that I'm ignoring the effect of the range of orbital radii <span class="math-container">$(1 \text{ AU } \pm R_\text{Hill})$</span> on the grain temperature (which is <span class="math-container">$\sim \pm 1\text{ K}$</span> from the central value).</li>
<li>the grains have modern Earth's albedo <span class="math-container">$A = 0.39 \leftarrow$</span> (probably the iffiest assumption, but I need an albedo and I had to start somewhere)</li>
<li>the star is the modern Sun with <span class="math-container">$L = L_\odot$</span></li>
</ul>
<p>Number of grains:</p>
<p><span class="math-container">$ N_g = \frac{M_\text{disk}}{m_g} = \frac{1 M_\oplus}{\rho_g \frac{4}{3}\pi r_g^3} = \frac{(5.97 \times 10^{24}\text{ kg})}{\frac{4}{3}\pi(5500 \text{ kg/m}^3)(5.0 \times 10^{-6} \text{ m})^3} \implies N_g = 2.08 \times 10^{36} $</span></p>
<p>Grain temperature:</p>
<p><span class="math-container">$ T_g = \left[\frac{L_\odot (1-A)}{16 \pi \sigma R_\text{orb}^2} \right]^{1/4} = \left[\frac{(3.83 \times 10^{26} \text{ W}) (1-0.39)}{16 \pi (5.67 \times 10^{-8} \text{ W/m}^2\text{K}^4) (1.50 \times 10^{11} \text{ m})^2} \right]^{1/4} \implies T_g = 246 \text{ K} $</span></p>
<p>Grain luminosity:</p>
<p><span class="math-container">$ L_g = 4 \pi \sigma r_g^2 T_g^4 = 4 \pi (5.67 \times 10^{-8} \text{ W/m}^2\text{K}^4) (5.0 \times 10^{-6} \text{ m})^2 (246 \text{ K})^4 \implies L_g = 6.54 \times 10^{-8} \text{ W} $</span></p>
<p>Protoplanetary disk luminosity:</p>
<p><span class="math-container">$ L_\text{disk} = N_g \cdot L_g = (2.08 \times 10^{36})(6.54 \times 10^{-8} \text{ W}) \implies \boxed{L_\text{disk} = 1.36 \times 10^{29} \text{ W}} $</span></p>
<p>If you've made it this far, thank you for your patience! I hope I've been sufficiently clear in my explanation; please let me know if I need to provide more information.</p>

<solar-system><planetary-formation><luminosity><proto-planetary-disk>
Protoplanetary disk luminosity - looking for a sanity check please
Chris M
# Protoplanetary disk luminosity - looking for a sanity check please

(Asked by: username_0 on 2023-03-05)

I've been told to "consider an Earth-mass of interplanetary grains (roughly spherical with a radius of a few microns) in a protoplanetary disk. Let the particles be in a torus with a cross-section of the Hill radius of the Earth, at a distance of $1 \text{ AU}$ from a $1M\_\odot$ protostar."

With this in mind, I must estimate the thermal velocity and mean time between collisions for the grains, and then compute the luminosity of the protoplanetary disk (ignoring any self-shadowing).

I'm content with my answer for thermal velocity & mean collision time, but the luminosity I get is:

$L\_\text{disk} = 1.36 \times 10^{29} \text{ W} \approx 350 ~L\_\odot$.

Now, given the dramatic size difference, I expected the disk to be more luminous than the Sun, but this struck me as excessive. **I'm hoping someone could please let me know if my methods are sound.**

(Obviously I am not asking anyone to do my homework for me, but rather to see if any assumption I've made stands out as utterly ridiculous or something along those lines. I've included my calculations to better demonstrate my thought process.)

My strategy was to consider the grains as collection of blackbody radiators and sum up their individual luminosities to obtain the disk's luminosity. I can estimate the equilibrium temperature of a grain using an assumed value for its albedo, which I can then use to calculate the re-radiated luminosity of each individual grain. I know the mass of the grains from their size and assumed density. I know the overall mass of the disk, so I can readily obtain the number of grains by dividing it by the grain mass. Multiplying the number of grains by their individual luminosity thus gives me the overall luminosity, since I'm told I can ignore self-shadowing.

My assumptions/simplifications:

* the grains are spherical and of radius $r\_g = 5 \mu\text{m}$
* the grains are composed of 'earthium' and therefore have the modern Earth's bulk density $\rho\_g = \rho\_\oplus = 5500 \text{ kg/m}^3$
* the grains have a uniform temperature $T\_g$, which is to say that I'm ignoring the effect of the range of orbital radii $(1 \text{ AU } \pm R\_\text{Hill})$ on the grain temperature (which is $\sim \pm 1\text{ K}$ from the central value).
* the grains have modern Earth's albedo $A = 0.39 \leftarrow$ (probably the iffiest assumption, but I need an albedo and I had to start somewhere)
* the star is the modern Sun with $L = L\_\odot$

Number of grains:

$ N\_g = \frac{M\_\text{disk}}{m\_g} = \frac{1 M\_\oplus}{\rho\_g \frac{4}{3}\pi r\_g^3} = \frac{(5.97 \times 10^{24}\text{ kg})}{\frac{4}{3}\pi(5500 \text{ kg/m}^3)(5.0 \times 10^{-6} \text{ m})^3} \implies N\_g = 2.08 \times 10^{36} $

Grain temperature:

$ T\_g = \left[\frac{L\_\odot (1-A)}{16 \pi \sigma R\_\text{orb}^2} \right]^{1/4} = \left[\frac{(3.83 \times 10^{26} \text{ W}) (1-0.39)}{16 \pi (5.67 \times 10^{-8} \text{ W/m}^2\text{K}^4) (1.50 \times 10^{11} \text{ m})^2} \right]^{1/4} \implies T\_g = 246 \text{ K} $

Grain luminosity:

$ L\_g = 4 \pi \sigma r\_g^2 T\_g^4 = 4 \pi (5.67 \times 10^{-8} \text{ W/m}^2\text{K}^4) (5.0 \times 10^{-6} \text{ m})^2 (246 \text{ K})^4 \implies L\_g = 6.54 \times 10^{-8} \text{ W} $

Protoplanetary disk luminosity:

$ L\_\text{disk} = N\_g \cdot L\_g = (2.08 \times 10^{36})(6.54 \times 10^{-8} \text{ W}) \implies \boxed{L\_\text{disk} = 1.36 \times 10^{29} \text{ W}} $

If you've made it this far, thank you for your patience! I hope I've been sufficiently clear in my explanation; please let me know if I need to provide more information.

**Tags:** solar-system, planetary-formation, luminosity, proto-planetary-disk

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## 1 answers

### Answer by username_1 on 2023-03-05. Score: 2

Yes, there's a major problem. You are trying to run a "device" that uses up $350L\_\odot$ with a $1L\_\odot$ power source. In fact it's worse than that because the grains cannot absorb more than a small fraction of the solar luminosity if they are concentrated into a torus. That cannot be an equilibrium situation.

Let's imagine the torus has a thickness of $0.1$ au. The surface area of the torus would be $1.4\times 10^{22}$ m$^2$, which represents only 5% of the surface area around the Sun at 1 au.

Your $2\times 10^{36}$ grains, each of radius $5\times 10^{-6}$ present a cross-sectional area of $1.6\times 10^{26}$ m$^2$, which is 500 times the available area at 1 au.

i.e. The assumption of no self-shadowing doesn't hold water; the torus would be optically thick; and the emitting area would be of order $10^4$ times lower.


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