Refractory (planetary science)

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

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]


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


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]


  1. ^ a b 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.
  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.
  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.