Help Shape the Future of Space Exploration

Join The Planetary Society Now Join Now!

Join our eNewsletter for updates & action alerts

   Please leave this field empty
Blogs

Headshot of Emily Lakdawalla

The Phoebe ring

Posted by Emily Lakdawalla

14-10-2009 16:06 CDT

Topics:

Sorry I'm late to this news, but as usual I'll try to compensate by being thorough! Last week, planetary astronomers Anne Verbiscer, Michael Skrutskie, and Doug Hamilton published a paper in Nature succinctly titled "Saturn's Largest Ring." In the paper, they announce the discovery, using the Spitzer infrared space telescope, of a gargantuan, previously unseen ring around Saturn, encompassing the orbit of Phoebe.

First, let's start with some background on the scale of Saturn's known rings. (Click here to skip the background and go straight to the Spitzer results.) You can measure the extent of the rings in kilometers, but astronomers and Cassini mission people both seem to find "Saturn radii" to be a handier unit that helps them have a better intuitive feel for the scale of things. One Saturn radius, abbreviated as R-subscript-s but usually written just as Rs to make things easier, is 60,330 kilometers. Beginning at Saturn's center, one radius gets you to Saturn's cloud tops. The main ring system, the part that's almost perfectly flat and aligned with Saturn's equator, includes the D, C, B, A, and F rings and is just a bit more than twice Saturn's diameter.

Saturn from above

NASA / JPL / SSI / Ian Regan

Saturn from above
On January 20, 2007 Cassini's orbit took it 60 degrees above the plane of the rings to capture this top-down view, composed of 12 separate wide-angle camera footprints. The resolution is about 77 kilometers per pixel. In the upper right corner of the image, Prometheus, Pandora, and Janus skirt the edge of the rings. This is the main ring system, from the thin braid of the F ring at outer edge, across the A ring to the densest B ring (which appears dark because we're looking at the unlit face here) into the C ring. The D ring is very faint and goes almost all the way down to Saturn's clouds.
Moving out from the main ring system, you get to the first ring that's extended vertically above and below the ring plane, and that's the G ring. In 2008, Cassini's imaging team discovered a tiny moon, now named Aegaeon, that orbits within it and is most likely the source of the material that makes up the G ring. Whenever rocks of any size smack into Aegaeon -- and there's plenty of such bodies wandering around the Saturn system, so such impacts are relatively frequent -- ejecta sprays off from the collision. Aegaeon is so tiny that its gravity is incredibly weak; the ejecta doesn't crash down to land back on the moon but instead winds up orbiting Saturn. The ejecta's orbit is pretty similar but not identical to Aegaeon's orbit, so you wind up with a ring of material composed of millions of tiny particles, each on its own orbit. The G ring extends to about 2.9 Rs
New moon of Saturn within the G ring: S/2008 S1

NASA / JPL / SSI

New moon of Saturn within the G ring: S/2008 S1
This series of images was captured by Cassini over a period of 10 minutes and follows the path of a newly discovered moonlet within Saturn's dusty G ring. The images were taken with long exposures, so background stars form streaks. At the same time, the ring was orbiting Saturn, so it is also streaked, but in the direction of orbital motion. Within the G ring in each image is a small streak of light: this is the reflected light of the moonlet S/2008 S1, now named Aegaeon. The images focus on an extremely tiny portion of the G ring, and when enlarged, show it at 7 kilometers per pixel. The moonlet itself is only about 500 meters across, far smaller than a single pixel in these images.
Next you get to the E ring. Unlike the G ring, which is dusty, and indeed unlike most rings observed anywhere in the solar system, the E ring is blue in color and composed predominantly of relatively uniformly sized particles of ice. It is enormous, going from about 3 Rs maybe all the way to the orbit of Rhea at almost 9 Rs. It varies in density, and is densest at the orbit of Enceladus, at 4 Rs. These characteristics of the E ring made planetary astronomers strongly suspect that some kind of internal geologic activity on Enceladus was supplying the E ring, and of course Cassini proved that surmise to be true.
Enceladus and the E ring

NASA / JPL / SSI

Enceladus and the E ring
With the Sun almost directly behind the view, the tiny moon Enceladus (slightly over 500 kilometers in diameter) is embedded in the E ring, which is created from the material spewed from Enceladus' south polar plumes. The view is down onto Enceladus' north; orbital motion is counterclockwise. The moon itself is the tiny dark spot in the ring; the much larger bright spot is the south polar plume. Some of the complex structure around Enceladus in the E ring results from different orbital speeds of ejected particles: slower particles lag behind (above) Enceladus, and wind up on larger orbits; faster particles stream ahead (below) Enceladus and wind up on smaller orbits. Other structures may result from interactions with Saturn's magnetic field.

And that's it; that's the extent of the ring system known before this discovery. It went out to about 9 Rs. Here's a photo of the ring system from Earth, taken during the last Saturn equinox and ring plane crossing in 1995. During the equinox, we see the rings edge-on, which makes it easier to spot faint rings using a telescope; their entire radial thickness is collapsed into one line across the sky, so you're effectively seeing a much thicker pile of dust.

Saturn's E ring

Institute for Astronomy, University of Hawaii

Saturn's E ring
This photo of Saturn was captured from a University of Hawaii telescope during the ring plane crossing on August 10, 1995. Saturn and its interior rings have been blocked from view so that their brightness won't wash out the image. The E ring is a very faint diagonal line extending to the left and right. On the E ring you can see four spots where icy moons reflected so much light that they saturated the camera's detector: from left to right, they are Rhea, Dione, Mimas, and Tethys.
E ring: 9 Rs. So when I say that the new ring discovered by Anne Verbiscer and her coworkers extends from 128 to 207 Rs, you should really be pretty amazed.

Most of Saturn's moons are part and parcel of the main ring system -- the E ring includes the orbits of Mimas, Enceladus, Tethys, Dione, and possibly Rhea. In terms of their distance from Saturn, you can think of them as the "single-digit-Rs" family. These moons all look pretty similar.

Beyond Rhea, the moons are suddenly spaced much farther apart, and have very different appearances. You have cloudy Titan and dark Hyperion at about 20 and about 24 Rs. Next comes two-faced Iapetus, which -- unlike all the moons I've listed so far -- has a notably inclined orbit and is all the way out at almost 60 Rs. This is the double-digit-Rs family.

Beyond Iapetus, there's another big gap and then you get to another totally different family. These moons tend to be very, very small, only a handful of kilometers in diameter, and they have inclined, eccentric orbits that are anywhere from roughly 200 to 400 Rs -- the triple-digit-Rs family. Their odd orbits have made astronomers suspect that they didn't form with Saturn but instead are captured wandering bodies -- Centaurs or even Kuiper belt objects. Standing out among these because of its size is Phoebe, which is 215 kilometers across, the only one that has ever been seen up close by a spacecraft.

The Cassini mission made special plans to fly past Phoebe during its cruise to Saturn; the encounter was on June 11, 2004. It was so far from Saturn that after sailing past Phoebe it took Cassini 19 more days to get to its rendezvous with Saturn for its orbit insertion!!

Phoebe

NASA / JPL / Space Science Institute

Phoebe
Cassini captured this view of Phoebe, which is made of two separate images, on June 11, 2004. The surface is covered with craters, and it appears that the moon was once nearly broken to bits by impacts that left huge gouges (at top and bottom). North is to the top. The center to lower right area looks brighter because the Sun is striking that part of the moon most directly.
All it takes is one glance at Phoebe to know that a lot of it has been blasted away due to numerous impacts with other, smaller bodies. So it is no stretch at all to imagine that, much as there is material in Aegaeon's orbit making the G ring, there should be material in Phoebe's orbit making a ring. Verbiscer and her coauthors predicted that there might be such a ring. But Phoebe's orbit is so incredibly large that this "ring" would be almost unimaginably sparse. It's so sparse that Cassini's instruments, wonderful though they are, have no hope of seeing the ring as any kind of object against black space.

But the Spitzer Space Telescope is a different story. In February of this year, Verbiscer and her colleagues pointed Spitzer's Multiband Imaging Photometer (MIPS) to image the region in several disconnected locations along Saturn's ecliptic plane all the way from Iapetus' orbit to 400 Rs at wavelengths of 24 and 70 microns.

What they found was "a diffuse double-peaked band of light coincident with Saturn's ecliptic plane." The band of light was found in an observation that spanned the region from 128 to 180 Rs. It was also seen in smaller snapshots that were centered on the outer moons Kiviuq (153 Rs) and Tarvos (180 Rs). Its presence was equivocal in an observation centered on Phoebe at 220 Rs. And there was no evidence for it in an observation centered at 400 Rs. Combining all these observations gives positive identification of the presence of the ring from 128 to 207 Rs, though its extent could be larger. The diagram below shows you the Spitzer observation that covers the region from 128 to 180 Rs.

Spitzer discovers ring in Phoebe's orbit around Saturn

NASA / JPL

Spitzer discovers ring in Phoebe's orbit around Saturn
In February 2009, the Spitzer Space Telescope pointed at Saturn and discovered a huge ring associated with the distant, irregular satellite Phoebe. Phoebe, at 107 kilometers across, is likely a captured body; it has a retrograde orbit around Saturn. Material blasted off of Phoebe by impacts of smaller bodies remains in Phoebe's neighborhood for millions to billions of years. Some of it spirals in toward Saturn and is swept up by Iapetus, Titan, and Hyperion.
The vertical thickness of the ring was observed to be about 40 Rs, and it has a curious double-peak in intensity -- that is, it's not thickest along Saturn's equator, but instead looks like two rings floating above and below Saturn's equator. Why does it look like that? This is actually one of the observations that ties it to Phoebe.

Phoebe has an elliptical orbit whose plane is inclined 5 degrees to Saturn's ecliptic (not equatorial!) plane. Bodies that are ejected from Phoebe but remain in Phoebe's orbit will share this 5-degree inclination. That means that they rise above and below the ring plane. Doing a little math using Phoebe's average orbital distance (215 Rs) and its orbital eccentricity (0.16) and its inclination (5 degrees) produces a prediction that the ring should be about 41 Rs thick, remarkably similar to the observation. Because the orbits precess with time, at different rates depending upon their average distance from Saturn, the orbiting ring particles spread to cover all possible spaces in which Phoebe orbits. This movie may help you understand the location and extent of the ring. Visit my Facebook page for the same in HD resolution.


o far, it's a cool result but it's sort of like stamp collecting -- we discovered a new X and described it, done. Where the paper gets really interesting is when the authors explore what happens to the particles in Phoebe's ring over time, something that you can model by writing down a few equations that describe the orbit of a particle, include Saturn, Phoebe, Iapetus, and Titan, include the masses, densities, and albedos of the particles, and the effects of incident sunlight.

What happens to particles depends upon their size. The biggest chunks, several centimeters in size or larger, don't really migrate anywhere, sticking around near Phoebe's orbit until they smack into something -- each other or Phoebe. The model simulation suggests that it would take more than the age of the solar system for half of the particles to be removed from the system by re-collision with Phoebe, so most of the biggest chunks are still out there somewhere in Phoebe's orbital space.

What about smaller particles? The article says "re-radiation of absorbed sunlight exerts an asymmetric force on dust grains, causing them to spiral in towards Saturn with a characteristic timescale of 1.5 x 105rg where rg is the particle radius in micrometers. This force brings all centimetre-sized and smaller material to Iapetus and Titan unless mutual particle collisions occur first....Most material from 10 micrometres to centimetres in size ultimately hits Iapetus, with smaller percentages striking Hyperion and Titan." This would be a slow process that has operated continuously since whenever Phoebe was captured into Saturn's orbit. There might have been bursts of material delivered to Iapetus associated with some of the bigger impacts that have left such large scars on Phoebe, but they would have been blips above a steady background.

Iapetus' leading hemisphere and 'snowman'

NASA / JPL / SSI / Emily Lakdawalla

Iapetus' leading hemisphere and 'snowman'
Cassini took this distant photo of Iapetus on November 27, 2006. On the left is the dark terrain of Cassini Regio, on Iapetus' leading hemisphere; toward the right, the dark material breaks up into a complicated boundary with the light terrain of Iapetus' trailing hemisphere. The eastern boundary of Cassini Regio is marked by a feature of three overlapping craters outlined in dark material that look a little like a snowman. The image has been enlarged by a factor of two, and the contrast adjusted to reveal more detail within the dark terrain, including two very large impact basins.
Anyone who knows the first thing about Iapetus should be saying "Aha!" at this point. Iapetus, is, of course, known for being the yin-yang moon, whose leading hemisphere is dark and whose trailing hemisphere is bright. Cassini observations of Iapetus have proven that the dark material is almost certainly exogenous (coming from outside) rather than endogenous (coming from internal geologic activity). The small number of fresh, rayed craters on Iapetus shows that the darkening process is continuing today. The fact that the dark stuff only shows up on the leading hemisphere -- the side of Iapetus that faces forward in its orbit -- suggests that it's "sweeping up" the dark material, plowing into it as it moves in its stately path around Saturn. The side of Iapetus that faces backward along its orbit is in the lee of Iapetus' motion through the cloud of particles and doesn't sweep up the material.

It's long been suggested that Phoebe could be the source of this dark material. Verbiscer et al. go on to do some calculations that suggest that Phoebe material accumulates on Iapetus at a rate of about 40 micrometers per million years; over the age of the solar system that gives you 20 centimeters of material deposited on Iapetus. But because there were probably once a lot more distant kilometer-scale moons of Saturn that eventually crashed into Phoebe, the production rate of Phoebe ring material and therefore the Iapetus accumulation rate in the past was very likely higher, "leading to...a cumulative thickness of material on Iapetus that is probably measured in metres."

It's all a pretty neat picture. It doesn't even require Phoebe to have any kind of unusual geologic activity or unusually large past impacts -- all it needs to be is a big body sitting in its distant orbit, and other bodies in the Saturn system will crash in to it and create this supply of material that eventually impacts Iapetus. One question I haven't answered yet though is how come Phoebe has a ring if such structures haven't been seen around other moons? For instance, someone asked me, why isn't there a dust ring around the orbit of our Moon?

In a way, the way we are finding fainter and fainter rings is parallel to the way we're finding smaller and smaller moons. I'm pretty certain that there are a few motes more dust along our Moon's orbit than there is outside our Moon's orbit, but the Moon is so large, with such strong gravity, that nearly everything that is ejected from any impact on the Moon almost immediately returns to the lunar surface; no one will ever find a "ring" in the Moon's orbit.

Clumps following Adrastea

NASA / JHUAPL / SwRI / annotation by E. Lakdawalla

Clumps following Adrastea
Jupiter's moon Adrastea has an associated ring. One of the surprising discoveries from New Horizons' encounter with Jupiter was three clumps in the main rings following the tiny moon Adrastea (16 kilometers in diameter). The image shown here was taken from an animation of the clumps moving around the rings (Quicktime format, 4 MB).
Elsewhere in the solar system, as you look to smaller and smaller moons, you will see more and more dust associated with that moon's orbit. In the Saturn system, the Cassini mission is careful as the spacecraft crosses the orbits of all the medium-sized moons like Tethys, Dione, and Rhea, pointing the high-gain antenna forward along its path so that the antenna acts like an umbrella, shielding the more sensitive instruments from collisions with little dust particles.

Look at the even smaller moons Thebe and Amalthea at Jupiter, and there are definite "gossamer rings" associated with their orbits. Interestingly, Verbiscer et al. point out in their paper that Thebe and Amalthea are "far more prolific sources of debris" than Phoebe because their close location to Jupiter means that collisions are more energetic, but because the debris from collisions re-impacts Thebe and Amalthea very quickly, the optical depth of their associated rings is actually very similar to the optical depth of the Phoebe ring, even though the Phoebe ring is far larger; which means that the Phoebe ring contains thousands of times more material than the Thebe and Amalthea gossamer rings do.

The article concludes: "Although [its] exotic properties as well as its sheer size make the Phoebe ring unique among known planetary rings, similar structures should also adorn the other gas giant planets." In other words, there's a lot more out there to be discovered!

Diagram of the Phoebe ring

NASA / JPL / SSI

Diagram of the Phoebe ring
The bulk of the ring material starts about six million kilometers (3.7 million miles) away from the planet and extends outward roughly another 12 million kilometers (7.4 million miles). The diameter of the ring is equivalent to 300 Saturns. The ring is also thick, about 20 Saturns across. It is tilted at about 27 degrees from the main ring plane and encompasses the orbit of the moon Phoebe. Both the ring and Phoebe orbit in the opposite direction of Saturn's other rings and most of its moons, including Titan and Iapetus.

 
See other posts from October 2009

 

Or read more blog entries about:

Facebook Twitter Email RSS AddThis

Blog Search

JOIN THE
PLANETARY SOCIETY

Our Curiosity Knows No Bounds!

Become a member of The Planetary Society and together we will create the future of space exploration.

Join Us

Featured Images

Hubble's view of Mars during the Comet Siding Spring flyby

Mars from Hubble STIS, April 26, 2012
Hubble's view of Mars on October 19, 2014 (color)
Mars as viewed by Hubble ACS/SBC, May 30, 2014
More Images

Featured Video

View Larger »

Space in Images

Pretty pictures and
awe-inspiring science.

See More

Join the New Millennium Committee

Let’s invent the future together!

Become a Member

Connect With Us

Facebook! Twitter! Google+ and more…
Continue the conversation with our online community!