As it flies past, the seven instruments on board will capture every moment of their fleeting encounter.
Over the months that follow, that data will trickle back to Earth, providing vital new clues to help piece together the story of our solar system’s formation and evolution.
But what do we already know about Pluto and its place in our solar system?
Most science is generally experimental in nature. If you want to find out how something works, you can hit it with a hammer, boil it in a test tube, or make it run through a complicated maze—you get the idea.
Astronomy, by contrast, is an observational science. We can’t really experiment (except through clever use of computers). Instead, we gather observations and use them to piece together the story of how, when, why, and where something happened.
So the universe is a crime scene, and astronomers are the detectives examining the clues left behind. Pluto, and its brethren in the space beyond the planets, are particularly important clues for astronomers studying our solar system’s past.
Pluto—A Celestial Oddball
In the years since it was discovered in 1930, astronomers have learned a great deal about Pluto. It’s turned out to be a very unusual object.
It is highly reflective, exuding a tenuous atmosphere when closest to the sun. In addition, it has a family of satellites, including the behemoth Charon, a little over 750 miles (1,200 kilometers) in diameter, it is just over half Pluto’s size.
Pluto’s orbit is distinctly non-circular, or eccentric. At its closest to the sun (a distance of 2.76 billion miles, or 4.44 billion kilometers), Pluto passes within the orbit of Neptune, while at its most distant it lies almost 1.8 billion miles (3 billion kilometers) further away.
Pluto’s orbit is also tilted, or inclined, by about 17 degrees to the plane of the solar system. Pluto wanders both far above and far below the other planets during each 248-year orbit.
The oddities don’t end there. Crossing paths with Neptune, you might expect Pluto to eventually come close to that planet, potentially even crashing into it. But it avoids such a fate due to something called a mean-motion resonance.
Pluto’s orbit takes around 50 percent longer than that of Neptune’s (164 years). Pluto therefore completes two full laps of the sun in around the time it takes Neptune to complete three. This prevents close encounters between Pluto and Neptune. Every time Pluto crosses Neptune’s orbit, Neptune is elsewhere.
It works like this: on the first orbit, Pluto beats Neptune to the point their orbits cross, and the two avoid a collision by a huge distance. By the time Pluto completes another orbit, Neptune has completed one and a half, meaning that it now precedes Pluto, and a collision is again avoided. After another Plutonian year, the two return to where they started, and the dance begins again.
Because Neptune completes three orbits in the time Pluto completes two, we say that they are trapped in 3:2 mean-motion resonance. And it is this resonance that is key to our understanding the solar system’s formation.
Pluto and Planet Formation
Our current best theory is that the solar system formed from a gas and dust-rich protoplanetary disk—much like those observed around young stars in the Orion nebula.
Hubblecast 32: The Proplyds in the Orion Nebula
For planets, dwarf planets and other assorted debris to form in such an environment, the disk has to be dynamically cold—in other words, as flat as a pancake.
In that scenario, the tiny fragments of dust and ice in the disk collide at such slow speeds that they can stick together, rather than smashing one another apart.
Fast forward uncounted collisions over a few tens of millions of years and a planetary system is born.
This is a surprisingly successful model and matches the clues we observe better than any of its rivals. But, at first glance, Pluto’s peculiar orbit seems to contradict the story. If Pluto formed that way, why does it now move on such an eccentric and inclined orbit?
And Pluto isn’t alone. We now know of a large population of objects beyond Neptune’s orbit, many of which are also trapped in resonance with Neptune, and move on inclined and/or eccentric orbits. They’re certainly not what you might expect of a population born from a thin, cold disk of material.
And so we have a clue, in the form of the eccentricities and inclinations of Pluto and the other Plutinos. But what does it portend?
Pluto as the Yardstick of Migration
As our models of planet formation have become more sophisticated, the simple picture that our planets formed on their current orbits has been overturned.
Based on the evidence frozen in to the solar system’s small body populations, we now think that Jupiter, Saturn, Uranus, and Neptune migrated as they grew, spreading out to reach their current dispersed architecture.
Neptune, in particular, was a great wanderer, with some models suggesting it formed between 600 million and 1.2 billion miles (between 1 billion and 2 billion kilometers) closer to the sun than we currently observe it. But how can we tell?
The answer? Pluto’s peculiar orbit and those of the Plutinos.
The Evidence for Neptune’s Great Journey
As the planets formed, with Neptune much closer to the sun than it is today, there was a wealth of debris (planetesimals) further out. As Neptune fed, devouring the material closest to it, it scattered material inward from this trans-Neptunian region and, in the process, began to drift outwards.
As Neptune moved, so did the location of its resonances. Objects were captured as the planet swept outwards, forced to move in lockstep with the giant.