Dear Wikiwand AI, let's keep it short by simply answering these key questions:
Can you list the top facts and stats about Frost line (astrophysics)?
Summarize this article for a 10 years old
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. Beyond the line, otherwise gaseous compounds (which are much more abundant) can be quite easily condensed to allow formation of gas and ice giants; while within it, only heavier compounds can be accreted to form the typically much smaller rocky planets.
Each volatile substance has its own frost line (e.g. carbon monoxide, nitrogen, and argon), so it is important to always specify which material's frost line is referred. A tracer gas may be used for materials that are otherwise difficult to detect; for example diazenylium for carbon monoxide.