Refractory (planetary science)

In planetary science, any material that has a relatively high equilibrium condensation temperature is called refractory.[1] The opposite of refractory is volatile.

The refractory group includes elements and compounds like metals and silicates (commonly termed rocks) which make up the bulk of the mass of the terrestrial planets and asteroids in the inner belt. A fraction of the mass of other asteroids, giant planets, their moons and trans-Neptunian objects is also made of refractory materials.[2]

Classification

The elements can be divided into several categories:

Category	Condensation temperatures	Elements
Super-refractory	higher than 1700 K	Re, Os, W, Zr and Hf
Refractory	between 1500–1700 K	Al, Sc, Ca, Ti, Th, Lu, Tb, Dy, Ho, Er, Tm, Ir, Ru, Mo, U, Sm, Nd and La
Moderately refractory	1300 to 1500 K	Nb, Be, V, Ce, Yb, Pt, Fe, Co, Ni, Pd, Mg, Eu, Si, Cr
Moderately volatile	1100–1300 K	Au, P, Li, Sr, Mn, Cu and Ba
Volatile	700–1100 K	Rb, Cs, K, Ag, Na, B, Ga, Sn, Se and S
Very volatile	less than 700 K	Pb, In, Bi and Tl

[1]

The condensation temperatures are the temperatures at which 50% of the element will be in the form of a solid (rock) under a pressure of 10⁻⁴ bar. However, slightly different groups and temperature ranges are used sometimes. Refractory material are also often divided into refractory lithophile elements and refractory siderophile elements.[3]

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gollark: Some of the non-programming people are doing hardware design somewhat, which is useful.

gollark: Only the computer science cohort of not many people is doing it, but due to scheduling only about 3 of us actually have significant programming experience.

gollark: We basically have that!

gollark: The competition is in March, it's totally* fine.

References

Taylor, Stuart Ross (2001). Solar system evolution: a new perspective : an inquiry into the chemical composition, origin, and evolution of the solar system. Cambridge University Press. pp. 73–75. ISBN 978-0-521-64130-2.
Beatty, J. Kelly (1999). Beatty, J. Kelly; Petersen, Carolyn Collins; Chaikin, Andrew (eds.). The new solar system. Cambridge University Press. pp. 314–315. ISBN 978-0-521-64587-4.
Davis, Andrew M.; Turekian, Karl K. (2005). Davis, Andrew M.; Holland, Heinrich D.; Turekian, Karl K. (eds.). Meteorites, comets, and planets. Elsevier. pp. 45–47. ISBN 978-0-08-044720-9.

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[Ross-1] Taylor, Stuart Ross (2001). Solar system evolution: a new perspective : an inquiry into the chemical composition, origin, and evolution of the solar system. Cambridge University Press. pp. 73–75. ISBN 978-0-521-64130-2.

[Beatty-2] Beatty, J. Kelly (1999). Beatty, J. Kelly; Petersen, Carolyn Collins; Chaikin, Andrew (eds.). The new solar system. Cambridge University Press. pp. 314–315. ISBN 978-0-521-64587-4.

[Davis-3] Davis, Andrew M.; Turekian, Karl K. (2005). Davis, Andrew M.; Holland, Heinrich D.; Turekian, Karl K. (eds.). Meteorites, comets, and planets. Elsevier. pp. 45–47. ISBN 978-0-08-044720-9.