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In astronomy or planetary science, the frost line, also known as the snow line or ice line, is the minimum distance from the central protostar of a solar nebula where the temperature is low enough for volatile compounds such as water, ammonia, methane, carbon dioxide and carbon monoxide to condense into solid grains, which will allow their accretion into planetesimals.
The boundary of the region where ice could form in the early Solar System is known as the frost line (or snow line), and is located in the modern asteroid belt, between about 2.7 and 3.1 astronomical units (AU) from the Sun. [24] [25] It is therefore necessary that objects forming beyond the frost line–such as comets, trans-Neptunian objects ...
An artist's illustration giving a simple overview of the main regions of a protoplanetary disk, delineated by the soot and frost line, which for example has been observed around the star V883 Orionis. [15] The nebular hypothesis of solar system formation describes how protoplanetary disks are thought to evolve into planetary systems.
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Planetesimals beyond the frost line accumulated up to 4 M E within about 3 million years. [39] Today, the four giant planets comprise just under 99% of all the mass orbiting the Sun. [b] Theorists believe it is no accident that Jupiter lies just beyond the frost line. Because the frost line accumulated large amounts of water via evaporation ...
The hot central protostar heats the surrounding dust disk so that, inside the frost line, the condensed ices sublimate, leaving the carbonaceous, silicate, and iron cores of the dust. Outside the frost line icy dust particles form comets and icy planetesimals. Within the disk, the motion of bodies smaller than 1 km is governed more by gas drag ...
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An additional difference is the composition of the planetesimals, which in the case of giant planets form beyond the so-called frost line and consist mainly of ice—the ice to rock ratio is about 4 to 1. [29] This enhances the mass of planetesimals fourfold.