The oxygen-isotope composition of chondrules and isolated forsterite and olivine grains from the Tagish Lake carbonaceous chondrite

Primordial oxygen isotope reservoirs of the solar nebula recorded in chondrules in Acfer 094 carbonaceous chondrite

“…A similar bimodal distribution has been observed in chondrules and isolated olivine grains from ALHA77307 (CO3) (Jones et al, 2000;Wasson et al, 2004), Murchison (CM2) (Jabeen and Hiyagon, 2003), Acfer 094 (Kunihiro et al, 2005), Y81020 (CO3) (Kunihiro et al, 2004;Tenner et al, 2011), Tagish Lake (C2-ungrouped) (Russell et al, 2010), and CR chondrites (Libourel and Chaussidon, 2011), although Connolly and Huss (2010) reported that type II chondrules from CR2 chondrites tend to have much higher D 17 O values. The Mg#s of the 16 O-rich group chondrules from Acfer 094 are mainly higher than 98 and the lower limit of the occurrence of the 16 O-rich group chondrules is at Mg# $ 96 (Fig.…”

Relict Olivines in Micrometeorites: Precursors and Interactions in the Earth’s Atmosphere

“…The present discussion is centered on understanding what types of precursors contribute to the Mg-rich grains in micrometeorites, and a comparison is made with the existing data for C1 (CI), C2 (CM), and C3 (CV) chondrites (Rubin & Wasson 1986;Steele 1986Steele , 1990Kurat et al 1989;Jones & Carey 2006;Russell et al 2010;Rudraswami et al 2011). Olivine is the dominant phase in chondrules, namely type I (FeO poor with Fa<10%) and II (FeO rich with Fa>10%), and the olivine varies in composition from Mg-rich to Mg-poor (Hewins 1997).…”

“…The rectangle is the region where thelikelihood of finding the particle within it is maximum. The data for chondrites are taken from theliterature (Rubin & Wasson 1986;Steele 1986Steele , 1990Kurat et al 1989Jones & Carey 2006Russell et al 2010;Rudraswami et al 2011). Forsteritic olivines in CI chondrites are rare and small in size (Steele 1990)and are closely associated with CM rather than CV chondrites (Steele 1985a(Steele , 1985b(Steele , 1990. Henceforth, data from the present study are compared only with CM and CV chondrites.…”

“…They concluded that micrometeorites are largely related to C2 The rectangle is the region where thelikelihood of finding the particle within it is maximum. The data for chondrites are taken from theliterature (Rubin & Wasson 1986;Steele 1986Steele , 1990Kurat et al 1989Jones & Carey 2006Russell et al 2010;Rudraswami et al 2011). chondrites, with some contribution of C3-and UOC-type chondrites. An overwhelming majority of forsterites from micrometeorites in the present study cluster in the narrow range shown by the rectangles in Figures 2 and 3, displaced slightly from C3 data and displaying an affinity to C2 forsterites, though not completely.…”

Multi-technique investigation reveals new mineral, chemical, and textural heterogeneity in the Tagish Lake C2 chondrite

“…Geochemical (Mittlefehldt, 2002;Nakamura et al, 2003), oxygen isotopic (Clayton and Mayeda, 2001;Baker et al, 2002;Russell, 2006;Russell et al, 2010), organic chemical (Pizzarello et al, 2001;Kminek et al, 2002;Binet et al, 2004), and petrologic (Zolensky et al, 2002) studies suggest a relationship between Tagish Lake and the CI and CM chondrites.…”