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How did the solar system begin forming

Planetary system formation coincides with the process of star formation in which our Sun belongs to the generation of stars created 4.6 billion years ago, when our galaxy was roughly half its present age. A cloud of interstellar gas, dust, and ices containing several generations of material collapsed to form the nebula from which the Sun and the rest of our solar system grew. This collapse may have been triggered by a nearby supernova. Cosmologists believe that because the material in the nebula was rotating to some degree, not all of the nebular material fell directly into the central mass that would become the Sun. Instead, some of the material was confined to a flat, spinning disk, called a protoplanetary disk, around a young Sun. As time went on, the grains and ices in the disk bumped into and stuck to one another forming macroscopic objects with sizes on of order 0.01-10 meters, all orbiting in the same direction and same plane analogus to the rings around Saturn. As the objects grew larger, their gravitational forces increased, attracting more matter from the disk and gradually building kilometer-sized bodies called planetesimals. These planetesimals further collided and either shattered into fragments or merged producing larger objects. The gravitational pull of the largest planetesimals produced rapid growth to the size of small planets and formed the nuclei of the planets as we know them today.

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