Evolution of protoplanetary disk inferred from 26Al chronology of individual chondrules

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The Non-carbonaceous–Carbonaceous Meteorite Dichotomy (2020, background): “The Al–Mg chronology of chondrules from ordinary, CV, and CO chondrites provide a narrow interval of formation ages of ∼ 2–3 Ma after CAI formation (Kita and Ushikubo 2012; Kunihiro et al. 2004; Kurahashi et al. 2008; Nagashima et al. 2017; Pape et al. 2019; Rudraswami and Goswami 2007; Rudraswami…”
The Compositional Structure of the Asteroid Belt (2015, methodology): “group could have the same age or a narrow range of ages) (Alexander and Ebel, 2012; Kita and Ushikubo, 2012), and that the youngest ages, indeed perhaps all chondrule ages, have been disturbed by parent body processes (Alexander, 2005; Alexander and Ebel, 2012).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “Kruijer et al. (2017) argue that Jupiter only grew to its current size 3-4 Myr after CAIs because carbonaceous chondrites continued to form until that time (Kita and Ushikubo, 2012; Connelly et al., 2012).”
Differentiated Planetesimals and the Parent Bodies of Chondrites (2013, background): “However, recent Al/Mg chronometry indicates that chondrule populations in individual ordinary and carbonaceous chondrite parent bodies formed over periods lasting ∼1–1.5 Ma, with the youngest chondrules originating 2.4 Ma or more after CAI formation (Hutcheon et al. 2009, Kita & Ushikubo 2011).”