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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.
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.
Jablonski diagram including vibrational levels for absorbance, non-radiative decay, and fluorescence.. When a molecule absorbs a photon, the photon energy is converted and increases the molecule's internal energy level.
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.
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 of the frost line. It depends on various factors, including the melt temperature, the speed of cooling, the extrusion speed, and the diameter of the bubble.
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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.
A Frost diagram or Frost–Ebsworth diagram is a type of graph used by inorganic chemists in electrochemistry to illustrate the relative stability of a number of different oxidation states of a particular substance.