Young giant planets are born from gas and dust. Researchers of ETH Zurich and the Universities of Zurich and Bern simulated different scenarios relying on the computing power of the Swiss National Supercomputing Centre (CSCS) to find out how they exactly form and evolve. They compared their results with observations and were able to show amongst others a big difference between the postulated formation mechanisms.
Astronomers set up two theories explaining how gaseous giant planets like Jupiter or Saturn could be born. A bottom-up formation mechanism states that first, a solid core is aggregated of roughly ten times the size of the Earth. “Then, this core is massive enough to attract a significant amount of gas and keep it,” explains Judit Szulágyi at the ETH Zurich and member of the Swiss NCCR PlanetS. The second theory is a top-down formation scenario: Here the gaseous disc around the young star is so massive, that due to self-gravity of the gas-dust, spiral arms are forming with clumps inside. Then, these clumps collapse via their own gravity directly into a gaseous planet, similar to how stars form. The first mechanism is called “core-accretion”, the second one “disc instability.” In both cases, a disc forms around the gas-giants, called the circumplanetary disc, which will serve as a birth-nest for satellites to form.
To find out which mechanism actually takes place in the universe, Judit Szulágyi and Lucio Mayer, Professor at the University of Zurich, simulated the scenarios on Piz Daint supercomputer at the Swiss National Supercomputing Centre (CSCS) in Lugano. “We pushed our simulations to the limits in terms of the complexity of the physics added to the models,” explains Judit Szulágyi: “And we achieved higher resolution than anybody before.”
In their studies, the researchers found a big difference between the two formation mechanisms: In the disc instability scenario the gas in the planet’s vicinity remained very cold, around 50 Kelvins, whereas in the core accretion case the circumplanetary disc was heated to several hundreds of Kelvins. “The disc instability simulations are the first that can resolve the circumplanetary disc around multiple protoplanets, using tens of millions of resolution elements in the computational domain. We exploited Piz Daint to accelerate the calculations using Graphics Processing Units (GPUs),” adds Mayer.
This huge temperature difference is easily observable. “When astronomers look into new forming planetary systems, just measuring the temperatures in the planet’s vicinity will be enough to tell which formation mechanism built the given planet,” explains Judit Szulágyi. A first comparison of the calculated and observed data seems to favour the core accretion theory. Another difference that was expected didn’t show up in the computer simulation. Before, astrophysics thought that the circumplanetary disc significantly differs in mass in the two formation scenarios. “We showed that this is not true,” says the PlanetS member.
Regarding the size of the new born planet, observations can be misleading as the astrophysicist found in a second study together with Christoph Mordasini, Professor at the University of Bern. In the core accretion model the researchers had a closer look at the disc around planets with masses three to ten times bigger than Jupiter’s. The computer simulations showed that gas falling on the disc from the outside heats up and creates a very luminous shock front on the disc’s upper layer. This significantly alters the observational appearance of young, forming planets.
“When we see a luminous spot inside a circumplanetary disc, we cannot be sure whether we see the planet luminosity, or also the surrounding disc luminosity,” says Judit Szulágyi. This may lead to an overestimation of the planet’s mass of up to four times. “So maybe an observed planet has only the same mass as Saturn instead of some Jupiter masses,” concludes the scientist.
In their simulations the astrophysicists mimicked the formation processes by using the basic physical laws such as gravity or the hydrodynamical equations of the gas. Because of the complexity of the physical models the simulations were very time consuming, even on Europe’s fastest supercomputer at CSCS: “On the order of nine months running time on hundreds to several thousands of computing cores,” estimates Judit Szulágyi: “This means that on one computing core it would have taken longer than my entire lifetime.”
Yet there are still challenges ahead. Simulations of disc instability still do not cover a long timescale. It is possible that after the protoplanet has collapsed to the density of Jupiter its disc will heat up more like in core-accretion. Likewise, the hotter gas found in the core-accretion case would be partially ionised, a favourable environment for effects of magnetic fields, completely neglected so far. Running even more expensive simulations with a richer description of the physics will be the next step.