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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.
[1] [2] [3] The term was borrowed from the notion of "frost line" in soil science and refers to the frosted appearance due to loss of transparency of the plastic film above the "frost line". [3] It is sometimes called freeze line, [3] while other disstinguish the concepts of frost/freeze line. [2] The distance from the die is called the height ...
In geology, the frost line is the level down to which the soil will normally freeze each winter. By an analogy, the term is introduced in other areas. Frost line (astrophysics), a particular distance in the solar nebula from the central protosun where it is cool enough for hydrogen compounds such as water, ammonia, and methane to condense into solid ice grains.
Because the frost line accumulated large amounts of water via evaporation from infalling icy material, it created a region of lower pressure that increased the speed of orbiting dust particles and halted their motion toward the Sun. In effect, the frost line acted as a barrier that caused the material to accumulate rapidly at ~5 AU from the Sun.
Frost diagram for manganese In electrochemistry , the tendency of two redox species to disproportionate, or comproportionate, can be determined by examining their Frost diagram . It is a graphical plot of nE ° = −Δ G °/ F as a function of the oxidation number for the different redox species of a given element.
The frost line—also known as frost depth or freezing depth—is most commonly the depth to which the groundwater in soil is expected to freeze. The frost depth depends on the climatic conditions of an area, the heat transfer properties of the soil and adjacent materials, and on nearby heat sources.
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Most liquids freeze by crystallization, formation of crystalline solid from the uniform liquid. This is a first-order thermodynamic phase transition, which means that as long as solid and liquid coexist, the temperature of the whole system remains very nearly equal to the melting point due to the slow removal of heat when in contact with air, which is a poor heat conductor.