Planet bulk chemistry

Swindle T. D., Kring D. A., Burkland M. K., Hill D. H., and Boynton W. V. (1998) Noble gases, bulk chemistry, and petrography of olivine-rich achondrites Eagles Nest and Lewis Cliff 88763 comparison to brachinites. Meteorit. Planet Sci. 33, 31-48. 

Barrat J. A., Blichert-Toft J., Nesbitt R. W., and Keller F. (2001) Bulk chemistry of Saharan shergottite Dar al Gani 476. Meteorit. Planet. Sci. 36, 23-29. 

Tiny solid cosmic particles - often referred to as dust - are the ultimate source of solids from which rocky planets, planetesimals, moons, and everything on them form. The study of the dust particles genesis and their evolution from interstellar space through protoplanetary disks into forming planetesimals provides us with a bottom-up picture on planet formation. These studies are essential to understand what determines the bulk composition of rocky planets and, ultimately, to decipher the formation history of the Solar System. Dust in many astrophysical settings is readily observable and recent ground- and space-based observations have transformed our understanding on the physics and chemistry of these tiny particles. 

Williams, Q. and Knittle, E., 1997. Constraints on core chemistry from the pressure dependence of the bulk modulus. Phys. Earth Planet. Interior, 100, 49-59. 

The earth s surface contains rocks and minerals, as well as clays and soils. The minerals may take many forms, including primary aluminosilicate minerals and other complex species that makeup the hard surface, or crust, of the planet. Aluminosilicates are made from aluminum, silicon, and oxygen and account for approximately 82% of the earth s crust by weight. Because of their structure, the soil surface chemistry is dominated by the reactions that occur on oxide and hydroxide-rich surfaces. These surfaces are extremely hydrophilic, layers of adsorbed water molecules surrounded by varying volumes of bulk water. 

---