### Compute Planet's Apparent Visual Magnitude

In a hypothetical solar system there exist:

- a sun of radius $r_s$ and absolute visual magnitude $V$
- the Earth, with radius $r_e$ and distance from the sun of $1\,AU$
- another planet, wit radius $r_p$, albedo $a$, distance from Earth $d_e$ (in units of $AU$), and distance from the sun $d_s$ ($AU$)

Assume that the second planet is magically lit up entirely by the sun (so it does not have phases when viewed from Earth).

Now how can I compute the apparent visual magnitude of the second planet with respect to Earth?

If there are other parameters required, please tell me.

@Aaron no, sorry. I'll edit the question.

@FlorinAndrei looking at that link, how can I compute the absolute magnitude $H$ of a planet?

Lets assume we're dealing with a superior planet, which is to say, the planet is orbiting at a greater distance than the Earth. This effectively ensures that there is no planetary phase to deal with.

Now, the Sun has a luminosity of $L_{sun}$ such that the Solar flux as seen by the planet is

$$

f_{planet} = \frac{ L_{sun} }{ 4 \pi d_s^2 }.

$$The cross section of the planet is about $A = \pi r_p^2$, so for a given albedo $a_p$ the reflective luminosity of the planet will be

\begin{aligned}

L_{planet} &= a_p f_{planet} A \\

&= a_p \pi r_p^2 \frac{ L_{sun} }{ 4 \pi d_s^2 }.

\end{aligned}Given that we know the absolute magnitude of the Sun, the absolute magnitude of the planet follows as

\begin{aligned}

V_{planet} &= -2.5 \log_{10}\left[ \frac{ L_{planet} }{ L_{sun} } \right] - V_{sun} \\

&= -2.5 \log_{10}\left[ a_p \frac{ r_p^2 }{ 4 d_s^2 } \right] - V_{sun}

\end{aligned}The apparent magnitude of the planet as seen from Earth can then be calculated as

$$

m_{planet} = V_{planet} + 5 \log_{10}\left[ d_{e-p} \right] - 5

$$

where the distance between Earth and the planet, $d_{e-p}$, should be in parsecs and of course depends on the orbital phase of the two respective planets.So the one additional parameter required was the Solar luminosity. There are probably a bunch of subtle effects with the albedo and the geometry of the system that are not taken into account here, but it should be a fair approximation.

Thanks for answering! One question, though: can solar luminosity not be computed from the sun's absolute visual magnitude (or the other way around) because the total luminosity does not have to all be in visual light? Or is there some other reason?

@feralin I guess you can, but you'd still need a second parameter to normalize the conversion, be it either the relative magnitude of the sun or an absolute magnitude of a calibration star. Using the relative magnitude of the sun would make sense here and probably gives a more direct final expression, but I think using luminosity gives a better sense of what's physically going on.

@feralin As a second note; if you want to model an inferior planet you can simply make the reflective surface - A - depend on (synodic) orbital phase.

sorry, but can you explain what "relative magnitude" is? I'm not getting good results from google...

@feralin sorry, I meant to say apparent magnitude

"the distance between Earth and the planet, de−p, should be in parsecs" is incorrect. For magnitudes within the solar system, distances must be in AUs. The formula reflects this in fact, since the absolute magnitude of a solar system object is defined at 1 AU viewing distance. The calculation of Vplanet is not affected, as long as rp and ds are expressed using the same unit of distance.

Is this albedo the Bond albedo or the Geometric albedo?

This appears to be incorrect, as it appears to predict that the apparent magnitude of the planet gets brighter as the Sun gets dimmer.

Planetary magnitudes vary not only according to the Sun’s luminosity, their own average albedo, and their distance from the Earth, but also from:

- Variations in their albedo across their surface.
- Their phase angle, for planets that we sometimes see as a crescent.
- Their inclination, for planets like Saturn and Uranus that have a different albedo at their equator than at their poles.
- Neptune keeps getting brighter. No one knows why.

All of these effects are detailed in an informative paper

*Computing Apparent Planetary Magnitudes for The Astronomical Almanac*by Mallama and Hilton, revised in 2018:https://arxiv.org/pdf/1808.01973.pdf

Their source code for computing planetary magnitudes given all of these effects can be found here:

https://sourceforge.net/projects/planetary-magnitudes/

Thanks for keeping Skyfield and Stack Exchange up to date!

just fyi I've just asked How fast is Neptune getting brighter? When was was this first noticed and reported?

If you want correct values, you have to take into account the effects mentioned in Brandon Rhodes' answer. Nevertheless, here's how to do a quick-and-dirty calculation.

The absolute magnitude of a planet is defined as the apparent magnitude if the Sun-planet and planet-observer distances are 1 au, at opposition.

Assuming a diffuse disc reflector model, the absolute magnitude $H$ of a planet of diameter $D_{\rm p}$ is given by

$$H = 5 \log_{10} \left( \frac{D_0}{D_{\rm p} \sqrt{a_p}} \right)$$

Where $a_p$ is the planet's geometric albedo, and $D_0$ is given by

$$D_0 = 2\,{\rm au} \times 10^{H_\ast / 5}$$

Where $H_\ast$ is the absolute magnitude defined at a reference distance of 1 au, which can be calculated from the usual 10 parsec absolute magnitude $M_\ast$ as follows:

$$H_\ast = M_\ast + 5 \log_{10} \left( \frac{1 \rm \ au}{10 \rm \ pc} \right) \approx M_\ast - 31.57$$

For the Sun, this results in $D_0 \approx 1329\ \rm km$.

To get the apparent magnitude of the planet, you can then use

$$m_{\rm p} = H + 5 \log_{10} \left( \frac{d_{\rm p\ast} d_{\rm po}}{1 \mathrm{\ au}^2} \right) - 2.5 \log_{10} q(\alpha)$$

Where $d_{\rm p\ast}$ is the distance between the planet and the star, $d_{\rm po}$ is the distance between the planet and the observer, and $q(\alpha)$ is the phase integral at the phase angle $\alpha$.

For the diffuse disc reflector, $q(\alpha) = \cos \alpha$. For a Lambertian sphere,

$$q(\alpha) = \frac{2}{3} \left( \left(1 - \frac{\alpha}{\pi} \right) \cos \alpha + \frac{1}{\pi} \sin \alpha \right)$$

At opposition, $\alpha = 0$, giving phase integrals of $q(0) = 1$ for the diffuse disc, and $q(0) = \tfrac{2}{3}$ for the Lambertian sphere.

Real planets have more complex phase functions which need to be determined empirically (see Brandon Rhodes' answer).

As a quick check, let's plug in values for Jupiter, taken from the NASA Jupiter Fact Sheet. With a (volumetric mean) diameter of 139,822 km and a geometric albedo of 0.538, the computed absolute magnitude is -9.44, versus the actual value of -9.40.

Using the computed value of -9.44, a distance from Jupiter of 5.204 au to the Sun and 4.204 au to the Earth, and using the Lambertian sphere $q(0) = \tfrac{2}{3}$, the apparent magnitude works out at -2.30, while for a diffuse disc $q(0) = 1$ the apparent magnitude works out at -2.74. The brightest the real planet gets is around -2.94. Fortunately for me, the value comes out in the right ballpark, despite the gross approximations being made to the reflection behaviour of real planets.

My computed values using $q(0) = 1$ for Saturn, Uranus and Neptune are 0.54, 5.57 and 7.75 respectively, which aren't too far off the real values either.

License under CC-BY-SA with attribution

Content dated before 7/24/2021 11:53 AM

Aaron 8 years ago

Do you also assume that the second planet is $d$ + 1 $\rm{AU}$ from the star?