# Why paint only one-half of Bennu?

The Gizmodo article Instead of Nuking an Asteroid Headed Toward Earth, We Could Just Splash It With Paint says:

“Even just painting the surface a different color on one half would change the thermal properties and change its orbit,” Michael Moreau, NASA’s OSIRIS-REx Flight Dynamics System Manager, told Gizmodo. That would involve literally sending a spacecraft to somehow change the color of some of the asteroid. (emphasis added)

Later it says:

Given the 120 years or so we’ve got and the amount of distance Bennu has left to travel before its nearby approach, if scientists could make some of it more susceptible to the solar radiation, that would slightly alter its path enough that it would miss us. Doing so would require changing part of its surface so it absorbs more radiation—for example, by covering one side of it with paint. Scientists first need to better study its orbit around the sun to determine the best course of action. (emphasis added)

Painting all of it would immediately increase decrease the magnitude of the average radial force it experiences from the Sun by roughly doubling the radiation pressure, altering its semi-major axis, period, and eccentricity by a small but well-defined amount. This is because both gravity and radiation pressure scale as $1/r^2$.

What is the physics behind choosing to paint only one half of the asteroid 101955 Bennu as mentioned twice in the article, rather than all of it? Would this be in any way better than painting all of it?

Quantitatively please, would painting half of Bennu be more effective than painting all of it in terms of it's potential Earth encounter in 2135? Or is this just to save on "space paint"?

• space.com/… Mar 21 '18 at 16:06
• Is there a paint that may be used successfully in the vacuum of space? Water or other usual solvents may not be used.
– Uwe
Mar 21 '18 at 20:20
• Painting only half of the asteroid should use the Yarkovsky effect.
– Uwe
Mar 21 '18 at 21:39
• @Uwe Yep, unless it's the "top" or "bottom" half. So then the question might be if that would be better than, or equivalent to painting the whole thing, quantitatively, as far as the 2135 close approach is concerned.
– uhoh
Mar 22 '18 at 0:12
• The problem with painting, or for that matter any approach which affects the asteroid while it's multiple AU away is that our current measurement systems cannot predict the final path accurately enough to know whether you're nudging it away or towards a collision. Jul 6 at 15:22

TLDR: It's not that painting half is optimum, it's that it's sufficient; you don't need more.

We know an amazing amount about 101955 Bennu and its orbit. D.S.Lauretta et al summarize this in their 2015 paper "The OSIRIS-REx target asteroid (101955) Bennu: Constraints on its physical,geological, and dynamical nature from astronomical observations" which includes this about the non-gravitational influence on it's existing orbit:

The Yarkovsky effect was found to be the most significant nongravitational acceleration acting to alter the asteroid’s orbit (Chesley et al. 2014). The Yarkovsky effect is a nongravitational thermal force that results from the way the asteroid rotation affects Bennu’s surface-temperature distribution. The absorption of sunlight, and its anisotropic thermal re-emission, can cause a small thrust (Chesley et al. 2003;Bottke et al. 2006). When thermal forces align with orbital velocity vectors, the Yarkovsky effect produces a steady drift in semimajor axis. Measurement of the Yarkovsky acceleration for Bennu is possible because we have obtained three precise series of radar ranging position measurements over a 12 yr period (ten orbits of Bennu around the Sun). The Yarkovsky effect produces a mean rate of change of Bennu’s semimajor axis of $-1.90(\pm0.01) \times 10^{-3} \rm{AU \: Myr}^{-1}$. Since first being observed in 1999, Bennu has drifted over 160 km as a result of this acceleration

So we have an measurement of the oft-discussed Yarkovsky effect on this asteroid. The effect is an force, hence acceleration, that depends a bit on distance from the Sun, but we can average that over each (slowly changing orbit). Note the displacement due to a constant acceleration grows quadratically with time: remember $d = 1/2 a t^2$?

That means between now and Bennu's close pass in 2135, the Yarkovsky effect moves Bennu by $(117 \rm{yr} / 18 \rm{yr})^2 \times 160\rm{km}$, or about 6,000 km.

The year 2135 pass is interesting because it's close enough to the Earth (0.003 AU) that Bennu's trajectory will be changed significantly. Depending on exactly how it's changed, that can bring Bennu into contact with Earth later on. Steven Chesley et al's 2014 paper "Orbit and Bulk Density of the OSIRIS-REx Target Asteroid (101955) Bennu" looks at this in great detail, identifying a large number of small "keyholes" that, if hit, will cause a later collision:

There are a lot of them, but they're all very very small compared to the 6,000km deflection due to the Yarkovsky effect. Note that zero isn't on the axis: Bennu isn't now aimed at any of them. The 2182 window is the closest, and the next one is 50,000km (note scale of figure) away.

If we had sufficiently accurate information, and determined that Bennu was headed for one of the keyholes, even a 20% change in the Yarkovsky effect would allow us to prevent a (much later) collision with Earth.

Even just painting the surface a different color on one half would change the thermal properties and change its orbit”

I think Moreau is aware of the size of the Yarkovsky effect, and realizes that only a (comparatively) small modification of it would be sufficient. So the "only .. half" is an expression of "we don't have to cover the whole thing 100% using a fine brush, we just have to modify the surface somewhat"

So it's not that "painting half of Bennu be more effective than painting all", it's that it's not necessary to do any more than painting half to move away from the (future) collision.

More detail on the orbital dynamics: The Yarkovsky effect in a specific case depends on the rotation of the asteroid. For a retrograde rotating (yes, we really know a lot about Bennu) asteroid, you can think of it as propulsive along the tangent to the orbit but against the motion. That's slowly lowering the orbit, lowering the semi-major axis by about $284 \pm 1.5 \rm{m/yr}$ (Chesley; note the sign should be negative in several places): If the Yarkovsky effect is increased, Bennu will be lower when it intersects Earth, closer to the Sun, though not necessarily closer to Earth. In the process, it's also changing the orbital period: this can add up over many orbits (many years) to make a much larger difference in position, which corresponds to a difference in arrive time at a point.

When working out whether a particular event, e.g. a keyhole passing, happens you have to consider both position and passage time. Chesley discusses this on page 17:

Table 5 details the effect of various differing models on the b-plane coordinates $(\xi_{2135},\zeta_{2135})$ of the close approach at the last reliably predicted Earth encounter for Bennu, which takes place in 2135. The b-plane is oriented normal to the inbound hyperbolic approach asymptote and is frequently used in encounter analysis. The (ξ,ζ) coordinates on the b-plane are oriented such that the projected heliocentric velocity of the planet is coincident with the −ζ-axis. In this frame the ζ coordinate indicates how much the asteroid is early (ζ < 0) or late (ζ > 0) for the minimum possible distance encounter. In absolute value, the ξ coordinate reveals the so-called Minimum Orbital Intersection Distance (MOID), which is the minimum possible encounter distance that the asteroid can attain assuming only changes to the timing of the asteroid encounter. For a more extensive discussion of these coordinates see Valsecchi et al. (2003) and references therein.

(Table continues in original paper with lots of rows for other really interesting effects, too) Comparing the $\Delta \xi$ value of a few tens of km and the $\Delta \zeta$ value of thousands of km shows that the largest effect is the delay: The Yarkovsky effects makes Bennu arrive late.

And that's why the horizontal axis of Fig 5 above is in terms of $\zeta_{2135}$; that's the delay that would change if you've changed the size of Bennu's Yarkovsky effect.

More detail on painting: White or black?

Either "white" or "black" paint would modify the size of the Yarkovsky effect on Bennu's orbit. From Lauretta et al:

The geometric visible albedo (pV) of Bennu is wellconstrained. Using the relationship 2.5 log pV =15.62 - 5 log D - H, where H is the absolute magnitude (from Hergenrother et al. 2013) and D the asteroid size (from Nolan et al. 2013), constrains pV to 4.5 +/- 0.5%. Applying a known correlation between the slope of the linear phase function and the albedo of asteroids (Belskaya and Shevchenko 2000; Oszkiewiczet al. 2011), yields an albedo of 3.0–4.5% based on Bennu’s phase function slope of 0.040 mag/deg (Hergenrother et al. 2013). Near-infrared spectroscopic data show a thermal tail longward of 2 microns (Fig. 5),consistent with an albedo of 4 +/1 1% (Clark et al. 2011). Spitzer photometric measurements combined with visible photometry constrain the albedo to 4.3 +/- 0.3% (Emery et al. 2014). OSIRIS-REx has adopted a geometric albedo of 4.5 +/- 0.5% for Bennu based on all of these independent determinations.

It's easier to raise a 4% albedo (with white paint) than to lower it (with black paint). But there's more to the question than that, because different paints require different amounts of mass to achieve coverage, have different procedures for application, etc. Both lighter and darker pigments have been studied: for example, S Ge and Hyland studied both carbon black (dark) and TiO2 (white). (See also Shen Ge thesis) Dark pigments tend to be more effective per kg of paint, but I don't think there's a complete understanding of all the alternatives. Research is continuing.

Which is better for avoiding a collision, more or less Yarkovsky effects?

It's important to note that right now, the answer is "neither". As far as we know, Bennu is not colliding with Earth in the next couple centuries. But we might be wrong: Extrapolating motion for that long is hard (take another look at the list of effects in Figure 5 of Lauretta et al). We could have it wrong. So at some time in the future, we might discover that Bennu is headed for Earth.

Most likely, that (eventual) collision will follow on an earlier Earth interaction that diverted Bennu to the collision. That's one of the keyholes mentioned above. In some sense, that makes the diversion problem simpler, but the extrapolation problem harder.

The diversion problem is simpler because a keyhole is much smaller than Earth. Typically a few km to maybe a couple hundred km wide, it takes much less of a change in orbit to miss one that to miss Earth. (You have a bit less time, due to the keyhole interaction being earlier, but generally the ratio of sizes is more important).

But note that if you modify the asteroid, you modify the path before and after the keyhole encounter: Worst case, you can miss the keyhole, but the asteroid will take a different path that now results in a different collision, and you've got to do the whole thing again with either more or less (!!) time to pull it off. Being able to predict those new paths accurately is very important.

So the mission planning is hard. We're getting better at predicting orbits (and asteroid perturbations), which is good. We have a bit of time AFAIK. And when we find that we really do need to modify an orbit to avoid a collision, that modification might involve either more or less Yarkovsky acceleration, so we might be sending out for either white or black paint.

• So the white paint reduces absorption, therefore heating, therefore directional blackbody radiation, therefore the magnitude of the Yarkovsky effect's impact on the rate of change of the semi-major axis. And so for the biggest bang for the buck one would paint the half between +/- 30 degrees latitude. This makes perfect sense!
– uhoh
Jul 1 '18 at 6:37
• I agree the exact math would be complicated. On this scale, where the perturbation is small compared to the size of the semi-major axis, the lowest expansion term in the differential motion pretty much has to be the quadratic one. Jul 1 '18 at 6:48
• See this paper for more on the specific geometry arxiv.org/pdf/1402.5573.pdf particularly figure 5 and the Minimum Orbit Intersection Distance methodology on page 17 which discusses minimum (possible) distance vs early/late (see table 5). (the $a$ in $da/dt$ in table 5 is the semi-major axis, not the acceleration $a$ in my answer above. I'll try to create some specific time vs offset numbers from that tomorrow. Jul 1 '18 at 7:04
• comment notes I may be wrong about the color of proposed "space paint". The Gizmodo article says "...if scientists could make some of it more susceptible to the solar radiation..." so I now assume they mean darker (and/or more emissive) than Bennu is now in visible and near-IR (or thermal) wavelengths. So I shouldn't have said "white paint" here.
– uhoh
Jul 1 '18 at 8:53
• @uhoh Added more discussion of time vs displacement and strengthen the argument about how far Bennu has to be displaced. Thanks for your help making the answer better. Jul 1 '18 at 16:49

The goal for painting the surface of the asteroid is not only to change the solar radiation pressure acting on the surface. The more likely reason is to alter the Yarkovsky effect on the asteroid (https://en.wikipedia.org/wiki/Yarkovsky_effect).

Yarkovsky effect is essentially anisotropic emmission of thermal protons. Since the emission is anisotropic, there is always a net momentum which can provide a very very tiny force on the asteroid. Now the goal of painting one half of the surface is to probably modify the surface temperauture of part of the surface and thereby increase the diurnal Yarkovsky effect (think night and day).

Interesting trivia: The mission Osiris-Rex will study this effect on Bennu.

You can read more on the concept in this Master's thesis: https://oaktrust.library.tamu.edu/bitstream/handle/1969.1/ETD-TAMU-2011-08-10184/GE-THESIS.pdf?sequence=2&isAllowed=y

• Ok, but the asteroid also rotates, thus the net effect of this Yarkovsky effect will be zero, isn't? Apr 1 '18 at 20:38
• @peterh no. The Yarkovsky effect is propulsive in nature. For example, the "hot" side heated by the Sun rotates backward and its thermal radiation produces thrust and a prograde acceleration. After a further half rotation, the side is facing the other way, but now it is cooler, and so does not produce a counter thrust of the same magnitude.
– uhoh
Apr 2 '18 at 2:01
• Thanks for your answer! I've asked Why paint only one-half... and Quantitatively please, would painting half of Bennu be more effective than painting all of it in terms of it's potential Earth encounter in 2135? Or is this just to save on "space paint"? because I'm interested in why (and if) using the Yarkovsky effect would be better than altering the radiation pressure.
– uhoh
Apr 2 '18 at 2:06
• Scolarpedia is more detailed about Yarkovsky effect. It contents underlaying math scholarpedia.org/article/Yarkovsky_and_YORP_effects Jun 29 '18 at 7:18
• @uhoh The Yarkovsky effect is only propulsive with a prograde rotating body. Bennu has a retrograde rotation, so because of this effect alone, it will spiral inward. Jun 29 '18 at 21:03

There is a strong economic reason to paint only one-half of Bennu.

With a mean radius of about 250 meters and a more or less spherical shape the surface area of Bennu is about 786,000 m$^2$.

One kg of paint could cover not much more than 20 m$^2$ surface area of Bennu, not taking into account the difficulty to cover the regolith.

This means a difference in mass of more than 18,000 kg of paint between covering one-half or the whole surface of Bennu.

It will be clear that, comparing with the nearly 4000 kg of the MSL spacecraft, at least 4 more spacecrafts would be required to carry the paint needed to cover the whole of Benno, above the initial 4 to cover "only" one-half.