Temporal Offsets Between Maximum CME Speed Index and Solar,Geomagnetic, and Interplanetary Indicators During Solar Cycle 23 and the Ascending Phase of Cycle 24     

A. Özgüç  A. Kilcik  K. Georgieva  B. Kirov 《Solar physics》2016,291(5):1533-1546

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Relationships Between Interplanetary Coronal Mass Ejection Characteristics and Geoeffectiveness in the Rising Phase of Solar Cycles 23 and 24   总被引：1，自引：0，他引：1  

M. Bendict Lawrance  A. Shanmugaraju  Y.-J. Moon  M. Syed Ibrahim  S. Umapathy 《Solar physics》2016,291(5):1547-1560

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Can a Fast-Mode EUV Wave Generate a Stationary Front?     

P. F. Chen  C. Fang  R. Chandra  A. K. Srivastava 《Solar physics》2016,291(11):3195-3206

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Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra     

A. A. Solov’ev  E. A. Kirichek 《Solar physics》2016,291(6):1647-1663

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Emission Measure and Temperature Analysis of the Upper Coronal Source of a Solar Flare     

Z. Ning  D. Li  Q. M. Zhang 《Solar physics》2016,291(6):1783-1798

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First Simultaneous Views of the Axial and Lateral Perspectives of a Coronal Mass Ejection     

I. Cabello  H. Cremades  L. Balmaceda  I. Dohmen 《Solar physics》2016,291(6):1799-1817

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North/South Hemispheric Periodicities in the >25 MeV${>}\,25\mbox{ MeV}$ Solar Proton Event Rate During the Rising and Peak Phases of Solar Cycle 24     

I. G. Richardson  T. T. von Rosenvinge  H. V. Cane 《Solar physics》2016,291(7):2117-2134

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Temporal Evolution of Solar Energetic Particle Spectra     

Donald J. Doran  Silvia Dalla 《Solar physics》2016,291(7):2071-2097

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Evidence for high‐temperature fractionation of lithium isotopes during differentiation of the Moon          下载免费PDF全文

James M. D. Day  Lin Qiu  Richard D. Ash  William F. McDonough  Fang‐Zhen Teng  Roberta L. Rudnick  Lawrence A. Taylor 《Meteoritics & planetary science》2016,51(6):1046-1062

Lithium isotope and abundance data are reported for Apollo 15 and 17 mare basalts and the LaPaz low‐Ti mare basalt meteorites, along with lithium isotope data for carbonaceous, ordinary, and enstatite chondrites, and chondrules from the Allende CV3 meteorite. Apollo 15 low‐Ti mare basalts have lower Li contents and lower δ⁷Li (3.8 ± 1.2‰; all uncertainties are 2 standard deviations) than Apollo 17 high‐Ti mare basalts (δ⁷Li = 5.2 ± 1.2‰), with evolved LaPaz mare basalts having high Li contents, but similar low δ⁷Li (3.7 ± 0.5‰) to Apollo 15 mare basalts. In low‐Ti mare basalt 15555, the highest concentrations of Li occur in late‐stage tridymite (>20 ppm) and plagioclase (11 ± 3 ppm), with olivine (6.1 ± 3.8 ppm), pyroxene (4.2 ± 1.6 ppm), and ilmenite (0.8 ± 0.7 ppm) having lower Li concentrations. Values of δ⁷Li in low‐ and high‐Ti mare basalt sources broadly correlate negatively with ¹⁸O/¹⁶O and positively with ⁵⁶Fe/⁵⁴Fe (low‐Ti: δ⁷Li ≤4‰; δ⁵⁶Fe ≤0.04‰; δ¹⁸O ≥5.7‰; high‐Ti: δ⁷Li >6‰; δ⁵⁶Fe >0.18‰; δ¹⁸O <5.4‰). Lithium does not appear to have acted as a volatile element during planetary formation, with subequal Li contents in mare basalts compared with terrestrial, martian, or vestan basaltic rocks. Observed Li isotopic fractionations in mare basalts can potentially be explained through large‐degree, high‐temperature igneous differentiation of their source regions. Progressive magma ocean crystallization led to enrichment in Li and δ⁷Li in late‐stage liquids, probably as a consequence of preferential retention of ⁷Li and Li in the melt relative to crystallizing solids. Lithium isotopic fractionation has not been observed during extensive differentiation in terrestrial magmatic systems and may only be recognizable during extensive planetary magmatic differentiation under volatile‐poor conditions, as expected for the lunar magma ocean. Our new analyses of chondrites show that they have δ⁷Li ranging between ?2.5‰ and 4‰. The higher δ⁷Li in planetary basalts than in the compilation of chondrites (2.1 ± 1.3‰) demonstrates that differentiated planetary basalts are, on average, isotopically heavier than most chondrites.  相似文献   

Petrology and oxygen isotopic compositions of clasts in HED polymict breccia NWA 5232          下载免费PDF全文

Katrina D. van Drongelen  Douglas Rumble III  Kimberly T. Tait 《Meteoritics & planetary science》2016,51(6):1184-1200

Northwest Africa (NWA) 5232, an 18.5 kg polymict eucrite, comprises eucritic and exogenic CM carbonaceous chondrite clasts within a clastic matrix. Basaltic clasts are the most abundant eucritic clast type and show a range of textures and grain size, from subophitic to granoblastic. Other eucritic clast types present include cumulate (high‐En pyroxene), pyroxene‐lath, olivine rich with symplectite intergrowths as a break‐down product of a quickly cooled Fe‐rich metastable pyroxferroite, and breccia (fragments of a previously consolidated breccia) clasts. A variable cooling rate and degree of thermal metamorphism, followed by a complex brecciation history, can be inferred for the clasts based on clast rounding, crystallization (and recrystallization) textures, pyroxene major and minor element compositions, and pyroxene exsolution. The range in δ¹⁸O of clasts and matrix of NWA 5232 reflects its origin as a breccia of mixed clasts dominated by eucritic lithologies. The oxygen isotopic compositions of the carbonaceous chondrite clasts identify them as belonging to CM group and indicate that these clasts experienced a low degree of aqueous alteration while part of their parent body. The complex evolutionary history of NWA 5232 implies that large‐scale impact excavation and mixing was an active process on the surface of the HED parent body, likely 4 Vesta.  相似文献