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We studied a unique super‐refractory inclusion with a core‐mantle structure from CO3.0 Yamato 81020 by secondary ion mass spectrometry, electron microprobe, and scanning electron microscope techniques. The core consists largely of hibonite and nonstoichiometric Al‐rich spinel indicating formation as a liquid at an exceptionally high temperature (>1900 °C). The mantle consists almost entirely of melilite with gehlenitic compositions (ranging from Åk2 to Åk25). The oxygen‐ and magnesium‐isotopic compositions of the core and mantle are very different; typically, Δ17O (≡δ17O − 0.52 δ18O) ~–26‰ and ƒMg (mass fractionation of Mg isotopes) ~10‰/amu in the core and Δ17O ~–7‰ and ƒMg ~1‰/amu in most of the mantle. The chemical and O, Mg‐isotopic data indicate that the core and mantle formed in separate events, and that the melilite now in the core was formed during the mantle‐melting event, probably filling preexisting voids and surficial cavities. Analyses of core and mantle phases plot along a single 26Al‐26Mg isochron with initial (26Al/27Al)0 corresponding to 4.8 ± 1.0 (±2σ) × 10–5, suggesting a similar formation age to normal CAIs in chondrites. [ABSTRACT FROM AUTHOR]

Background: Human fibroblast growth factor-2 (rhFGF-2) therapy has been used for periodontal tissue regeneration. However, few studies have reported their adjunctive procedures based on strategy of tissue engineering. The aim of this retrospective study is to assess the adjunctive effects of modified papilla preservation technique (mPPT) and combination with autogenous bone grafts (AG) on the rhFGF-2 therapy.Methods: Total of 44 sites underwent rhFGF-2 therapies and the evaluations in the survey periods. The primary outcome was set to the radiographic bone fill by radiographic examinations at 6 and 12 months after surgeries. We analyzed the correlation between influencing factors and the primary outcome, and differences of therapeutic effect by combination therapy with mPPT and that with AG.Results: After surgeries, probing depth (PD), clinical attachment level (CAL) and bone defects significantly improved. The improvements of radiographic bone fill were significantly positive correlated with a number of bone walls, combination with mPPT, and AG at 6 months after surgeries, and with combination with mPPT and AG at 12 months after surgeries. The significant differences of improvements of radiographic bone fill were demonstrated between combination with or without mPPT at 12 months after surgeries, and with or without AG at 6 and 12 months after surgeries. Moreover, the multiple linear regression analysis for the radiographic bone fill indicated the significant regression coefficient with conducts of mPPT.Conclusions: mPPT and AG had powerfully adjunctive effects on rhFGF-2 therapy. Further studies are needed in order to verify by randomized clinical trials. [ABSTRACT FROM AUTHOR]

Coarse‐grained, igneous Ca‐Al‐rich inclusions (CAIs) in CV chondrites formed through multiple melting events. We conducted in situ O‐isotope analysis and Al‐Mg systematics by secondary ion mass spectrometry of relict and overgrown minerals from a partial melting event in an Allende Type B CAI, Golfball. Golfball has a Type B CAI bulk composition and a unique structure: a fassaite‐rich mantle enclosing a melilite‐rich core. Many of the blocky melilite crystals in the core have irregularly shaped, Al‐rich (Åk5–15) cores enclosed in strongly zoned (Åk30–70) overgrowths. Since the Al‐rich melilite grains could not have formed from a melt of Golfball, they are interpreted as relict grains that survived later melting events. The O‐isotopic compositions of the blocky melilite crystals plot along the carbonaceous chondrite anhydrous mineral line, ranging between Δ17O ~ −14‰ and −5‰. The Al‐rich relict melilite grains and their overgrowths exhibit the same O‐isotopic compositions, while the O‐isotopic compositions are varied spatially among melilites. We found that the O‐isotopic compositions steeply change across several melilite crystals within few tens of micrometers, indicating the O‐isotopic compositions of the melt could not have been homogenized during the partial melting in that scale. According to the time scale of O self‐diffusivity in the melt, the cooling rate of the partial melting event is calculated to be >6 × 104 K h−1. Al‐Mg isotope data for core minerals plot on a straight line on an Al‐Mg evolution diagram. A mineral isochron for Golfball gives initial 26Al/27Al of (4.42 ± 0.20) × 10–5 and initial δ26Mg* of −0.035 ± 0.050‰. The chemical and O‐isotopic compositions of melilite and those initial values imply that its precursor consisted of fluffy Type A and/or fine‐grained CAIs. The partial melting event for Golfball may have occurred in very short order after the precursor formation. [ABSTRACT FROM AUTHOR]

A planetary mantle after core formation has been thought to be highly depleted in carbon due to its strong siderophile behavior. However, the carbon contents in lunar and terrestrial mantles are much greater than experimental predictions; thus, how the carbon contents in terrestrial mantles were established is puzzling and poorly understood. Here, we present high‐pressure experiments on the metal‐silicate partitioning of carbon at 2 GPa and 1923 K in a system containing 0.2 wt% C, which is close to that in enstatite chondrites, and show that a magma ocean made of chondritic materials is nearly saturated with carbon even under metal saturation. The consistency between the solubility of carbon in silicate melts and the carbon contents in lunar and terrestrial mantles also supports a nearly carbon‐saturated magma ocean during core formation and suggests that carbon contents in terrestrial mantles may have been established during the main accretion phase. Plain Language Summary: Carbon had played a key role on the evolution of planetary climate, mantle, and the origin of life. However, how the carbon content in the Earth's mantle has been established remains still poorly constrained. Here, we report the core‐mantle partitioning of carbon under chondritic carbon concentrations and carbon‐saturated conditions. The results show that the mantle of planetary embryos during core formation may have been nearly saturated with carbon. The consistency of carbon contents between the solubility of carbon in silicate melts under metal saturation and lunar and terrestrial mantles supports this hypothesis. Our results indicate that the carbon contents in planetary mantles may have been controlled mainly by the compatibility of carbon with silicate melts and determined during the main accretion of planetary embryos. Key Points: The effect of carbon concentrations on the liquid metal‐silicate partitioning of carbon was experimentally investigatedMagma oceans of planetary embryos made of enstatite chondrites may have been nearly saturated with carbon even under the presence of metallic liquidsThe solubility of carbon in silicate melts is very consistent with the carbon contents in lunar and terrestrial mantles [ABSTRACT FROM AUTHOR]

CM chondrites are a group of primitive meteorites that have recorded the alteration history of the early solar system. We report the occurrence, chemistry, and oxygen isotopic compositions of P-O-rich sulfide phase in two CM chondrites (Grove Mountains [GRV] 021536 and Murchison). This P-O-rich sulfide is a polycrystalline aggregate of nanometer-size grains. It occurs as isolated particles or aggregates in both CM chondrites. These grains, in the matrix and in type-I chondrules from Murchison, were partially altered into tochilinite; however, grains enclosed by Ca-carbonate are much less altered. This P-O-rich sulfide in Murchison is closely associated with magnetite, FeNi phosphide, brezinaite (Cr3S4), and eskolaite (Cr2O3). In addition to sulfur as the major component, this sulfide contains ~6.3 wt% O, ~5.4 wt% P, and minor amounts of hydrogen. Analyses of oxygen isotopes by SIMS resulted in an average δ18O value of −22.5 ‰ and an average Δ17O value of 0.2 ± 9.2 ‰ (2σ). Limited variations in both chemical compositions and electron-diffraction patterns imply that the P-O-rich sulfide may be a single phase rather than a polyphase mixture. Several features indicate that this P-O-rich sulfide phase formed at low temperature on the parent body, most likely through the alteration of FeNi metal (a) close association with other low-temperature alteration products, (b) the presence of hydrogen, (c) high Δ17O values and the presence in altered mesostasis of type-I chondrules and absence in type- II chondrules. The textural relations of the P-O-rich sulfide and other low-temperature minerals reveal at least three episodic-alteration events on the parent body of CM chondrites (1) formation of P-O-rich sulfide during sulfur-rich aqueous alteration of P-rich FeNi metal, (2) formation of Ca-carbonate during local carbonation, and (3) alteration of P-O-rich sulfide and formation of tochilinite during a period of late-stage intensive aqueous alteration. [ABSTRACT FROM AUTHOR]

- The oxygen isotopic microdistributions within melilite measured using in situ secondary ion mass spectrometry correspond to the chemical zoning profiles in single melilite crystals of a fluffy type A Ca-Al-rich inclusions (CAIs) of reduced CV3 Vigarano meteorite. The melilite crystals show chemical reverse zoning within an individual single crystal from the åkermanite-rich core to the åkermanite-poor rim. The composition changes continuously with the crystal growth. The zoning structures suggest that the melilite grew in a hot nebular gas by condensation with decreasing pressure. The oxygen isotopic composition of melilite also changes continuously from 16O-poor to 16O-rich with the crystal growth. These observations suggest that the melilite condensation proceeded with change consistent with an astrophysical setting around the inner edge of a protoplanetary disk where both 16O-rich solar coronal gas and 16O-poor dense protoplanetary disk gas could coexist. Fluffy type A CAIs could have been formed around the inner edge of the protoplanetary disk surrounding the early sun. [ABSTRACT FROM AUTHOR]

A melilite‐rich, compact type A Ca‐Al‐rich inclusion (CAI), KU‐N‐02, from the reduced CV3 chondrite Northwest Africa 7865, is mantled by an åkermanite‐poor layer. We carried out a combined study of petrographic observations and in situ O and Al–Mg isotopic measurements for KU‐N‐02. The core shows a typical texture of igneous compact type A CAIs. The mantle consists of spinel, åkermanite‐poor melilite, and perovskite. Individual mantle melilite crystals show reverse zoning toward the crystal grain boundary, in contrast to core melilite crystals showing normal zoning. The O isotopic compositions of the minerals in KU‐N‐02 plot along the carbonaceous chondrite anhydrous mineral line on a three O‐isotope diagram. The mantle and core spinel crystals are uniformly 16O‐rich (Δ17O ~ −23‰). The mantle melilite crystals exhibit variable O isotopic compositions ranging between Δ17O ~ −2‰ and −9‰, in contrast to the uniformly 16O‐poor (Δ17O ~ −2‰) core melilite. The mantle melilite crystals also exhibit variable δ25Mg values (δ25MgDSM‐3 ~ −2‰ to +3‰) compared with the nearly constant δ25Mg values of the core melilite (δ25MgDSM‐3 ~ +2‰). The mantle minerals are likely to have formed by condensation from the solar nebular gas after core formation. The Al–Mg mineral isochrons of the core and mantle give initial 26Al/27Al ratios of (4.66 ± 0.15) × 10−5 and (4.74 ± 0.14) × 10−5, respectively. The age difference between the core and mantle formation is estimated to be within ~0.05 Myr, implying that both melting and condensation processes in the variable O isotopically solar nebular environments occurred within a short time during single CAI formation. [ABSTRACT FROM AUTHOR]