Manganese solar abundance

Natural isotopes of manganese and their solar abundances... 

The agreement between meteoritic and solar abundances must be considered excellent and there is not much room left for further improvements. Obvious candidates for redetermination of the solar abundances are manganese and sulfur. 

The abundances of 39 nongaseous elements in the Sun have assigned errors below 30%. Only the four elements sulfur, manganese, scandium, and strontium differ by more than 20% from Cl abundances. The difference is below 10% for 27 of these elements. The agreement between meteoritic and solar abundances must therefore be considered excellent and there is not much room left for further improvements. Obvious candidates for redetermination of solar abundances are manganese and sulfur. The hmiting factor in the accuracy of meteorite abundances is the inherent variability of Cl chondrites, primarily the Orgueil meteorite. 

The concentrations of four typical moderately volatile elements—manganese, sodium, selenium, and zinc—in the various classes of chondritic meteorites are shown in Figure 12, where elements are normalized to magnesium and CI-chondrites. Again there is excellent agreement between solar abundances and Cl-meteorites. A characteristic feature of the chemistry of carbonaceous chondrites is the simultaneous depletion of sodium and manganese in all types of carbonaceous chondrites, except Cl. Ordinary and enstatite chondrites are not or only slightly... 

Calculations along these lines have been performed by Blackwell et at. (1972) using experimentally determined gf-values. When the results were compared with the measured equivalent widths of the manganese solar absorption lines they obtained a solar abundance of... 

The proportions with respect to iron of vanadium-51, manganese-55 and cobalt-59, formed as manganese-51, cobalt-55 and copper-59, respectively, also agree with abundances observed in the Solar System. The overall coherence of this behaviour suggests that appropriate conditions for synthesis of iron peak elements should be sought in... 

Direct measurements of the initial abundance of 53Mn in the early solar system have proven unreliable. CAIs, the first solids to form in the early solar system, are highly depleted in both manganese and chromium, both of which are moderately volatile. Operationally, the relative 53Mn-53Cr timescale has been anchored to an angrite, LEW 86010 (see above). Age differences have been calculated relative to LEW 86010 from... 

Based on the bulk chemistry, IDPs are divided into two groups (i) micrometer-sized chondritic particles and (ii) micrometer-sized nonchondritic particles. A particle is defined as chondritic when magnesium, aluminum, silicon, sulfur, calcium, titanium, chromium, manganese, iron, and nickel occur in relative proportions similar (within a factor of 2) to their solar element abundances, as represented by the Cl carbonaceous chondrite composition (Brownlee et al., 1976). Chondritic IDPs differ significantly in form and texture from the components of known carbonaceous chondrite groups and are highly enriched in carbon relative to the most carbon-rich Cl carbonaceous chondrites (Rietmeijer, 1992 Thomas et al., 1996 Rietmeijer, 1998, 2002). 

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