Calculating the luminosity of a comet

Question

Assuming a 9-km comet is heading towards the Earth and it is at distance 5.2 AU away from the Sun, what is its luminosity? Assume that it has an albedo of 0.5?

For now, I have calculated the Sun's flux at the comet's location.

$$F=\frac{3.8\times10^{26}W}{4\pi\left(7.78\times10^{11}m\right)^2}=50.74\frac{W}{m^2}$$

I have used the flux of the Sun and the distance of the comet from the Sun to the in meters. I was thinking that I could calculate the area of the comet seen from the Earth and then calculate the luminosity of the comet. However, I have no idea how to calculate the effective area of the comet.

Answer 1

I believe, givn the paucity of information in the question, that what is meant is that if the comet is only visible by virtue of light it reflects, then what is its luminosity.

This can be calculated from how much light it receives, which is given by the flux of sunlight at its position (which you have calculated), multiplied by its cross-sectional area, which is $\pi r^2$, where $r$ is the comet radius. A fraction $A$, where $A$ is the albedo, is then reflected. i.e. $$L \simeq A \pi r^2 \left( \frac{L_\odot}{4\pi d^2}\right)\, , $$ where $d$ is the distance from the Sun.

If instead the question is asking what the intrinsic luminosity of the comet is by virtue of it being heated by the sunlight then you would have to make all sorts of assumptions about whether it is in equilibrium or not (doubtful), whether it is heating up or cooling down, whether there is sublimination from the surface, and then possibly what its temperature is, and have a model for its emissivity.

If it were in equilibrium and you could assume that everything it absorbs is re-emitted (rather than say going into powering sublimation) then $$ L \simeq (1-A)\pi r^2 \left( \frac{L_\odot}{4\pi d^2}\right)\, , $$ which for $A=0.5$ is exactly the same answer ($A=0.5$ is a huge overestimate of the albedo of a cometary nucleus by the way).

Answer 2

We can calculate the luminosity "H" (absolute magnitude) by means of:

$$H=5 \ \log \frac{1329}{d \cdot \sqrt p}$$

log is the decimal logarithm

d is the diameter in km

p is the albedo

For d=9 km and p=0.5 we obtain H=11.6

We cannot calculate the apparent luminosity, since the distance to Earth is not given. If we knew the distance to the Earth, then we could calculate the apparent luminosity (apparent magnitude) by means of:

$$m=H+5 \ \log (D_s \cdot D_e)-2.5 \ \log f(F)$$

m is the apparent magnitude

Ds is the distance to the Sun in Astronomical Units (AU)

De is the distance to Earth in Astronomical Units (AU)

f(F) is the phase function

For more details, consult:

Will the James Webb Space Telescope be visible from earth?

and:

Good source for the relationship between absolute magnitude, diameter, and albedo?

Answer 3

Geez… only antlersoft gets it. AmeliaGrace wants the effective cross-sec of the comet , not a nucleus , which would be straightforward. A comet is a phenomenon of nucleus plus coma plus tail plus whatever adnexa. (Ulysses showed that tails, at multiple comets, are ridiculously long. A human notion of “tail” is limited by our eyesight, not what’s actually there or not.)

The extent of a coma, let alone tail, is inherently arbitrary- Rosetta flying through 67P/C-G’s coma was “filthy” by spacecraft-engineering standards but still cleaner than a cleanroom on Earth. The definition/calculation of coma radius/tail length then arbitrates with instrument aperture, exposure time, etc. And that was 67P/C-G. ‘Oumuamua was dust-poor, gas-rich to the point that its very comethood could only be showed mathematically, not directly observed (imaging) at all. And there is every shade of grey between these two extremes- 2/Encke, for one, is considered “dust-poor” because its solid emission is mainly macroscopic grains, which violate the standard for “dust” and show up poorly in most telescopes.

Faced with a continuum debate, the simplest path forward is to define some line in the sand, then proceed with that (arbitrary) standard, acknowledging its limited domain. AmeliaGrace even started down this trail in the woods:

I was thinking that I could calculate the area of the comet seen from the Earth

Assuming visible-light telescopes/detectors, this is somewhat straightforward. If there’s an issue, it’s an arbitrary line separating faint coma from noise/hot pixels, but we do that already, no choice but to. Even then, that line is drawn at different radii, for active comets versus comets still in the outer Solar System versus comets just not releasing much.

However, I have no idea how to calculate the effective area of the comet.

Given a comet, go ahead and take the image and draw your radius. But for comet s , you cannot give the radii of their whole class .