This chemistry reveals new insights into the conditions of the planet-forming disc surrounding this young star. “With ALMA we can directly observe this chemistry in discs that are right now in the process of making planets,” said Karin Öberg, an astronomer at the Harvard-Smithsonian Center for Astrophysics in Cambridge, Mass., and lead author on a paper published in the Astrophysical Journal. “The molecules have formed two spectacular rings. The inner one we expect to see; the outer one comes as a complete surprise and sheds new light onto the properties of a protoplanetary disc’s outer reaches.”
The presence of a DCO+ ring nearest to the star, the astronomers note, comes from the right combination of low temperatures and abundant carbon monoxide (CO) gas, which is essential for the formation of DCO+. Closer to the star, conditions are too warm for DCO+ to form. Further out, the entire reservoir of CO freezes out, forming a layer of ice on dust grains and planetesimals.
The presence of the outer ring implies that farther and farther from the star it not only gets colder and darker, as would be expected, but it also hits a point where the disc density is so low that some light from the host star can penetrate down to the midplane of the disc. This replenishes the reservoir of CO gas and restarts the production of DCO+. Heavy, deuterium-based molecules can thus form in more places around young stars than previously thought. This increases the utility of these molecules to tell us about the history of both our solar system and other planetary systems in the making.
“Heavy molecules are, in fact, interstellar messengers that tell us how and where different types of molecules form,” noted Öberg. “For example, based on an excess of heavy water in the Earth’s oceans we know that most of the Earth’s water comes from the pre-solar nebula, so it’s actually older than the Sun!”
