Advanced Mineralogy: Volume 3: Mineral Matter in Space, by Arnold S. Marfunin

By Arnold S. Marfunin

This quantity of complex Mineralogy encompasses six various parts having gains in universal: they're with regards to one of many biggest organizations of the second one half this century; and signify the last word and ultimate extension of the concept that of mineral topic. - figuring out mineral topic in area is among the critical reasons of cosmic exploration. This comprises the result of compa­ rative planetology, lunar epopee, subtle meteorite experiences (now greater than 500 meteorite minerals), discovery of the interstellar mineral dirt forming a few 60 trillion of earth plenty within the Galaxy, and terrestrial effect crater experiences. it truly is attainable now to talk of mineralogy of the Universum, and the mineralogical form of the states of topic within the Universe. Direct samples of mantle xenoliths and ultrahigh pressure-tem­ perature experiments give the chance to think about the mineral­ ogical composition of the Earth as a complete, together with the higher an reduce mantle and the Earth's center. Deep ocean drilling courses, a systematic fleet of hundreds and hundreds of vessels and several other submersibles have led to nice dis­ coveries within the geology, metalogeny, and mineralogy of the sea ground the biggest a part of the Earth's floor, particularly revealing new genetic, crystallochemical, and ore sorts of min­ eral formation.

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The hydrous minerals contain some elements in chondritic abundances (e. , Ti, AI, Cr, Na, K). Chapter 1. Mineral Matter in Space 30 Antarctic Micrometeorites Olivine EMPA . 8 .... 0+-~--~--~~·r---~~A-----r-----4 o 10 20 30 FeO (wt%) 40 50 Fig. 10. Plot ofCr2 0 3 vs. %) of olivines from micrometeorites which have varying FeO contents and commonly high Cr20 3 contents (terrestrial olivines usually do not contain Cr). 5 wt% FeO, which are common in CM and CR chondrites, are very rare in MMs Refractory minerals like Mg-Al spinel are strongly enriched in refractory trace elements (e.

Under different interstellar conditions the gas may be molecular, atomic, or ionized, with temperatures anywhere from less than 10 to over 106 K. In the vicinity of the solar system, gas atoms are separated from each other by distances of the order of 1 cm, while individual dust particles are separated from each other by hundreds of meters. Because interparticle collisions occur so infrequently, the gas and dust are not necessarily in thermal equilibrium with each other. The dust temperature ranges from less than 10K in dense molecular clouds, to over 1000 K in stellar winds and in the vicinity of newly forming stars.

Nature 332: 611623 Buerki PR, Lentwyles S (1991) Homogeneous nucleation of the diamond powder by CO 2-laser-driven gas-phase reactions. J Appl Phys 69: 3739-3744 Clayton DD (1989) Origin of heavy xenon in meteorite diamonds. Astrophys J 340:613619 Fisenko AV, Verchovsky AB, Semjonova LF (1994) Noble gases in the interstellar diamond of Efremovka CV3 chondrite. Geokhimia N7: 916-927 (in Russian) Fisenko AV, Tatsy VF, Semjonova LF, Bolsheva LN (1995) Experimental studies of oxidation kinetics of the meteoritic diamonds by air oxygen.

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