Frost Line: The Boundary That Shaped the Planets

Frost Line: The Invisible Frontier That Sculpted the Solar System

The frost line, or snow line, represents the critical distance from the Sun at which volatile compounds such as water, ammonia, carbon dioxide, and methane can condense into ice. This thermodynamic boundary played a decisive role in the formation and differentiated composition of the planets.

The frost line is located approximately at 2.7 AU for water in the Solar System, but this value varies depending on the Sun's luminosity. It separates regions where solid matter is dominated by rocks from those where ice becomes abundant, influencing the size and composition of the planets. The position of the frost line is determined by the balance between the radiant flux of the young Sun and the ability of molecules to condense.

For water, the frost line is around 170 K (-103°C), the temperature at which water vapor condenses directly into ice in the vacuum of space. This critical temperature corresponds to a heliocentric distance of about 3 AU in the primordial Solar System.

Role in Planet Formation

The frost line fundamentally influenced the architecture of our Solar System:

• Terrestrial planets: Inside the frost line, only refractory materials (silicates, metals) could accrete, forming small rocky planets.
• Gas giants: Beyond the frost line, abundant ices allowed the formation of more massive planetesimals, capable of rapidly accreting large gaseous envelopes.
• Asteroid belt: Located near the frost line, it has a mixed composition with rocky asteroids (S-type) and carbonaceous asteroids (C-type) containing hydrates.

Temporal Evolution of the Frost Line

The frost line is not fixed over time. Its position has evolved throughout the history of the Solar System depending on solar luminosity, the temperature of the protoplanetary disk, and internal dynamic processes. During the early stages of formation, when the Sun was less luminous, the frost line was closer to the Sun.

Over time, as solar luminosity increased and the disk gas dissipated, the frost line moved outward, changing the condensation zone of water and other volatile compounds. This migration had a direct impact on the mass that planets could accumulate and on the distribution of icy bodies.

• Early phase: frost line closer to the Sun, condensation of water, and initial formation of terrestrial planets and the first icy planetesimals.
• Intermediate phase: gradual outward movement, favoring the growth of gas giants and the accumulation of ice on asteroids and comets.
• Current phase: approximate stabilization at 2.7 AU for water, with extensive icy zones in the Kuiper Belt and beyond.

This temporal evolution explains why some planets and satellites contain large amounts of ice despite their relatively close current position to the Sun, and why the distribution of icy bodies is not uniform.

Table: Comparison of Condensable Compounds

Sources: NASA Solar System Formation.