| Jul 31, 2024 |
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(Nanowerk News) Our solar system is our immediate cosmic neighborhood. We know it well: the Sun at the center; then the rocky planets Mercury, Venus, Earth, and Mars; and then the asteroid belt; followed by the gas giants Jupiter and Saturn; then the ice giants Uranus and Neptune; and finally the Kuiper belt with its comets. But how well do we really know our home?
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Previous theories have assumed that giant planets are formed by collisions and accumulations of asteroid-like celestial bodies, so-called planetesimals, and the subsequent accretion of gas over the course of millions of years. However, these models explain neither the existence of gas giants located far from their stars nor the formation of Uranus and Neptune.
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| Artist’s impression of a young star surrounded by a protoplanetary disc made of gas and dust. Ring-shaped, turbulent disturbances (substructures) in the disk lead to the rapid formation of several gas and ice giants. (Image: LMU / Thomas Zankl, crushed eyes media)
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From grain of dust to giant planet
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Astrophysicists from LMU, the ORIGINS cluster, and MPS have developed the first ever model to incorporate all the necessary physical processes that play a role in planet formation. Using this model, they have shown that annular perturbations in protoplanetary disks, so-called substructures, can trigger the rapid formation of multiple gas giants. The results of the study (Astronomy & Astrophysics, “Sequential giant planet formation initiated by disc substructure”) match the latest observations and indicate that the formation of giant planets could happen more efficiently and quickly than previously thought.
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With their model, the researchers demonstrate how millimeter-sized dust particles accumulate aerodynamically in the turbulent gas disk, and how this initial perturbation in the disk traps dust and prevents it from disappearing off in the direction of the star. This accumulation makes the growth of planets very efficient, as suddenly a lot of “building material” is available within a compact area and the right conditions for planet formation are present.
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“When a planet gets large enough to influence the gas disk, this leads to renewed dust enrichment farther out in the disk,” explains Til Birnstiel, Professor of Theoretical Astrophysics at LMU and member of the ORIGINS Cluster of Excellence. “In the process, the planet drives the dust – like a sheepdog chasing its herd – into the area outside its own orbit.”
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The process begins anew, from inside to outside, and another giant planet can form.
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“This is the first time a simulation has traced the process whereby fine dust grows into giant planets,” observes Tommy Chi Ho Lau, lead author of the study and doctoral candidate at LMU.
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Variety of gas giants in our and other solar systems
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In our solar system, the gas giants are situated at a distance of around 5 astronomical units (au) (Jupiter) to 30 au (Neptune) from the Sun. For comparison, the Earth is some 150 million kilometers from the Sun, which is equivalent to 1 au (which is equivalent to the average distance from the Earth to the Sun – approximately 150 million kilometers).
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The study shows that in other planetary systems, a perturbation could set the process in motion at much larger distances and still happen very rapidly. Such systems have been observed frequently in recent years by the ALMA radio observatory, which has found gas giants in young disks at a distance beyond 200 au. However, the model also explains why our solar system apparently stopped forming additional planets after Neptune: the building material was simply used up.
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The results of the study match current observations of young planetary systems that have pronounced substructures in their disks. These substructures play a decisive role in planet formation. The study indicates that the formation of giant planets and gas giants proceeds with greater efficiency and speed than previously assumed. These new insights could refine our understanding of the origin and development of the giant planets in our solar system and explain the diversity of observed planetary systems.
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