Astronomical observations reveal that protoplanetary disks around young stars commonly have ring- and gap-like structures in their dust distributions. These features are associated with pressure bumps trapping dust particles at specific locations, which simulations show are ideal sites for planetesimal formation. Here we show that our Solar System may have formed from rings of planetesimals—created by pressure bumps—rather than a continuous disk. We model the gaseous disk phase assuming the existence of pressure bumps near the silicate sublimation line (at T ~ 1,400 K), water snowline (at T ~ 170 K) and CO snowline (at T ~ 30 K). Our simulations show that dust piles up at the bumps and forms up to three rings of planetesimals: a narrow ring near 1 au, a wide ring between ~3–4 au and ~10–20 au and a distant ring between ~20 au and ~45 au. We use a series of simulations to follow the evolution of the innermost ring and show how it can explain the orbital structure of the inner Solar System and provides a framework to explain the origins of isotopic signatures of Earth, Mars and different classes of meteorites. The central ring contains enough mass to explain the rapid growth of the giant planets’ cores. The outermost ring is consistent with dynamical models of Solar System evolution proposing that the early Solar System had a primordial planetesimal disk beyond the current orbit of Uranus.

天文观测表明，年轻恒星周围的原行星盘在其尘埃分布中通常具有环状和间隙状结构。这些特征与在特定位置捕获尘埃颗粒的压力颠簸有关，模拟显示这些位置是小行星形成的理想场所。在这里，我们展示了我们的太阳系可能是由小行星环形成的——由压力颠簸产生——而不是一个连续的圆盘。我们假设在硅酸盐升华线（在T  ~ 1,400 K）、水雪线（在T  ~ 170 K）和 CO 雪线（在T ~ 30 K)。我们的模拟表明，尘埃堆积在凸起处并形成多达三个小行星环：1 au 附近的窄环、~3-4 au 和 ~10-20 au 之间的宽环和 ~20 au 和〜45 au。我们使用一系列模拟来跟踪最内环的演化，并展示它如何解释太阳系内部的轨道结构，并提供一个框架来解释地球、火星和不同类别陨石的同位素特征的起源。中央环的质量足以解释巨行星核心的快速增长。最外圈与太阳系演化的动力学模型一致，提出早期太阳系在天王星当前轨道之外有一个原始小行星盘。