benzylidene-1,3-dithio-malonic acid S,S'-diethyl ester | 16695-08-2

• 分子结构分类: 有机化合物 - 苯丙烷和聚酮 - 肉桂酸及其衍生物
• 英文名称: benzylidene-1,3-dithio-malonic acid S,S'-diethyl ester
• 英文别名: Benzyliden-dithiolmalonsaeure-diethylester；benzylidene-1,3-dithio-malonic acid S,S'-diethyl ester；Benzyliden-1,3-dithio-malonsaeure-S,S'-diaethylester
• CAS: 16695-08-2
• 化学式: C₁₄H₁₆O₂S₂
• 分子量: 280.412
• InChiKey: SBXUHPQIHKBGCM-UHFFFAOYSA-N

计算性质

• 辛醇/水分配系数(LogP)：
  3.63
• 重原子数：
  18.0
• 可旋转键数：
  5.0
• 环数：
  1.0
• sp3杂化的碳原子比例：
  0.29
• 拓扑面积：
  34.14
• 氢给体数：
  0.0
• 氢受体数：
  4.0

反应信息

• 作为产物：
  描述：

  S,S'-diethyl dithiomalonate 、 苯甲醛 在 ammonium acetate 作用下， 以 溶剂黄146 、 苯 为溶剂， 生成 benzylidene-1,3-dithio-malonic acid S,S'-diethyl ester
  参考文献：
  名称：

  Scheithauer,S.; Mayer,R., Chemische Berichte, 1967, vol. 100, # 5, p. 1413 - 1427

  摘要：

  DOI：

文献信息

• Evidence for low-temperature growth of fayalite and hedenbergite in MacAlpine Hills 88107, an ungrouped carbonaceous chondrite related to the CM-CO clan
  作者：Alexander N. KROT、Adrian J. BREARLEY、Michael I. PETAEV、Gregory W. KALLEMEYN、Derek W. G. SEARS、Paul H. BENOIT、Ian D. HUTCHEON、Michael E. ZOLENSKY、Klaus KEIL

  DOI：10.1111/j.1945-5100.2000.tb01522.x

  日期：2000.11

  Abstract— The carbonaceous chondrite MacAlpine Hills (MAC) 88107 has bulk composition and mineralogy that are intermediate between those of CO and CM chondrites. This meteorite experienced minor alteration and a low degree of thermal metamorphism (petrologic type 3.1) and escaped post‐accretional brecciation. The alteration resulted in the formation of fayalite (Fa90–100). Al‐free hedenbergite (∼Fs50Wo50), phyllosilicates (saponite‐serpentine intergrowths), magnetite, and Ni‐bearing sulfides (pyrrhotite and pentlandite). Fayalite and hedenbergite typically occur as veins, which start at the opaque nodules in the chondrule peripheries, crosscut fine‐grained rims and either terminate at the boundaries with the neighboring fine‐grained rims or continue as layers between these rims. These observations suggest that fayalite and hedenbergite crystallized after accretion and compaction of the fine‐grained rims. Fayalite also overgrows isolated forsteritic (Fa1–5) and fayalitic (Fa20–40) olivine grains without any evidence for Fe‐Mg interdiffusion; it also replaces massive magnetite‐sulfide grains. The initial 53Mn/55Mn ratio of (1.58 ± 0.26) × 10−6 in the MAC 88107 fayalite corresponds to an age difference between the formation of fayalite and refractory inclusions in Allende of either ∼9 or 18 Ma, depending upon the value of the solar system initial abundance of 53Mn used in age calculations.Formation of secondary fayalite and hedenbergite requires mobilization and transport of Ca, Si, and Fe either through a high‐temperature gaseous phase (Hua and Buseck, 1995) or low‐temperature aqueous solution (Krot et al., 1998a, b). The high‐temperature nebular model for the origin of fayalite (Hua and Buseck, 1995) fails to explain (a) formation of fayalite‐hedenbergite assemblages after accretion of fine‐grained rims that lack any evidence for high‐temperature processing; (b) extreme fractionation of refractory lithophile elements of similar volatility, Ca and Al, in hedenbergite; and (c) absence of Fe‐Mg interdiffusion along fayalite‐forsterite boundaries. We conclude that fayalite and hedenbergite in MAC 88107 formed during late‐stage, low‐temperature (approximately 150–200 °C) aqueous alteration. The data for MAC 88107 extend the evidence for an early onset of aqueous activity on chondrite parent bodies and reinforce the conclusion that liquid water played an important role in the chemical and mineralogical evolution of the first chondritic planetesimals.