Title: Making the Planetary Material Diversity During the Early Assembling of the Solar System
Authors: Francesco C. Pignatale, Sébastien Charnoz, Marc Chaussidon, Emmanuel Jacquet
Status: Accepted to ApJL, 2018 [open access]
The younger ones dared each other to go right up to the edge and look out. They hoped for spectacle, for storms or flames or bolts of lightning, but the view was peaceful. Calmer, even, than home.
Why can’t we go?, they asked the elders again. Nothing happens there. We’d come right back.
You’re right, the elders replied, that nothing happens. Nothing happens at all. That’s why you must not go.
Why? they asked. Why?
Because when nothing happens, you gather dust, the elders said. In a place where nothing happens, try as you might, that’s all you can ever do again.
The early days of the Solar System, like much of what happens in space, were indeed spooky. We know this because (a) there’s a Monster Mash verse about it and (b) like all great spooky scenes, they’ve left behind enduring mysteries.
For one: how did the oldest meteorites, which contain minerals that form at very high temperatures and minerals that form at much lower temperatures, come to be? More specifically, how did those minerals get all mixed up together in the first few thousand years of the Solar System?
There are a couple of clues: firstly, as is rare in astronomy, we can actually run lab tests on meteorites and measure their ages very precisely with radiometric dating. We therefore know that the atomic building blocks which would eventually end up in the meteorites (in the form of “calcium-aluminum-rich inclusions,” or CAIs) formed extremely quickly, before the Sun’s birth cloud was even done collapsing into the protoplanetary disk.
Secondly, we have observations of nearby young stars in the Milky Way which tell us that, as a star’s birth cloud collapses and condenses to form a protostar, dust and crystalline solids form around the protostar at the same time. It’s good external confirmation of what meteorites tell us happened around the baby Sun.
Simulating the Beginning
Today’s authors take this picture of a protoplanetary disk evolving even as the star’s big spherical birth cloud is still collapsing, and simulate it in the simplest possible terms. They start with a small disk with a source of light and heat at the center (to represent the protostar), and then they let a big spherical gaseous envelope gradually collapse into the disk.
They keep track of the temperature of the dust and gas at each point and use it to calculate what’s going on chemically—which molecules are vaporized by high temperatures, which are heated and chemically changed by intermediate temperatures, which condense due to cold temperatures. Their goal is to understand how the mixture of minerals contained in meteorites came to be—in particular, how did the CAIs, which form very early and at high temperatures, get mixed up with the much cooler, later-forming minerals that surround them in meteorites?
There are a number of physical effects that influence the presence and mixing of these minerals. First, there’s the question of temperature—heat propagates outward from the protostar at the center, meaning that the disk is hottest in the middle and coolest at its outer edge. As time progresses, the cloud continues to collapse from the inside out, so the radius at which dust from the collapsing cloud arrives in the disk moves outward. Hence, the temperature greeting this arriving dust gets cooler over time: at first, the dust arrives near the center of the disk and is instantly vaporized, but later on, it might only be chemically changed by the heat, or even later, might survive unscathed. (The disk spreads out over time, too, meaning that material that was initially close to the star and very hot can cool and condense later on.)
Second, there’s the question of turbulence. Some parts of the disk are calmer than others—in particular, there’s a “dead zone” (d̵̦̼͐ͅe̷̛̠̝͉̮͋̎͛̉̾̚͜͝͝a̷͖̮̔̈́͂̀͝d̵̗̗̩̭̑͗̊̈͐̕̚ ̸̛̺͔͕̪̖͊̈́̂̀̓̾̋z̴̮̝̗̼̓̇̊̓́̀̎̿o̵̭͆̇̆n̴̫̺̩̎̿ę̷͍̪̲̞͓͛ͅ) of extremely low turbulence, marked by the darker gray zone in figures 2 and 3. Dust and gas that arrives in the dead zone tends to stay there, because it’s not turbulented (a word, I posit) away, while dust and gas that arrive in the turbulent zones get all turbulented around (still a word).
Finally, there’s the question of accretion onto the protostar, which is happening throughout the disk evolution—in particular, gas interior to the dead zone is strongly accreted, and it tends to take the solids in that region (like CAIs) with it. Solids which are accreted onto the star cannot, of course, go on to become meteorites.
After 1.5 million years of evolution, the simulation successfully reproduces the mixing between CAIs and other minerals that must have produced the meteorites: the region of the disk with the highest CAI concentration is the same region with a lot of unprocessed dust, or dust that formed at cold temperatures and was never heated and chemically changed. Figure 3 illustrates this point–out past 10 AU, all three types of mineral coexist.
Success for a simple (spooky) solar system model!