Marina A. Ivanova, Michael K. Weisberg<\/p>\n\n\n\n
MAPS, Version of Record online: 20 October 2026<\/p>\n\n\n\n
LINK<\/strong><\/a><\/p>\n\n\n\n “These comments are devoted to our observations based on recently reviewing publications regarding reduced ungrouped chondrites (F-, HH, and others). In these publications, the authors defined a group of \u201cF-chondrites,\u201d comprising previously ungrouped chondrites of petrologic types 3 and 4 that exhibit very low fayalite (Fa) content. One publication concluded that certain reduced chondrites belonged to the F-group based solely on cluster analysis, disregarding previously published petrologic data for these meteorites. We propose that the meteorites classified as F-chondrites in these publications actually comprise at least two distinct groups: the F-chondrites and metal-rich, matrix-free chondrites of the \u201cG\u201d group. The average olivine composition in F-chondrites is Fa4.06\u2009\u00b1\u20091.48\u2009mole%, whereas in G-group chondrites it is Fa0.70\u2009\u00b1\u20090.43\u2009mole%. Notably, it is impossible to determine the petrologic type of G-group chondrites due to differences in the evolution and thermal history of their parent asteroid, and reduced chondrites, also G chondrites and reduced chondrites are very different in texture and petrography.”<\/p>\n\n\n\n Reply to comments on the publication \u201cA statistical investigation into the relationships between the IIE irons and the ordinary, F and \u201cHH\u201d chondrites.\u201dMeteoritics & Planetary Science 60, 2376\u20132400<\/strong><\/a><\/p>\n\n\n\n R. S. Kirby, P. L. King, A. G. Tomkins<\/p>\n\n\n\n MAPS, Version of Record online: 05 October 2026<\/p>\n\n\n\n
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