deca-2c,8c-diene-4,6-diyne | 483370-46-3

• 分子结构分类: 有机化合物 - 碳氢化合物 - 不饱和烃
• 英文名称: deca-2c,8c-diene-4,6-diyne
• 英文别名: Deca-2c,8c-dien-4,6-diin；Deca-2c,8c-dien-4,6-diin；(2Z,8Z)-deca-2,8-dien-4,6-diyne
• CAS: 483370-46-3
• 化学式: C₁₀H₁₀
• 分子量: 130.189
• InChiKey: CYAHDZCGTZPNJD-GLIMQPGKSA-N

计算性质

• 辛醇/水分配系数(LogP)：
  3.1
• 重原子数：
  10
• 可旋转键数：
  1
• 环数：
  0.0
• sp3杂化的碳原子比例：
  0.2
• 拓扑面积：
  0
• 氢给体数：
  0
• 氢受体数：
  0

反应信息

• 作为反应物：
  描述：

  deca-2c,8c-diene-4,6-diyne 在 lead 、 钯 作用下， 生成 deca-2c,4c,6c,8c-tetraene
  参考文献：
  名称：

  Heavily-hydrated lithic clasts in CH chondrites and the related, metal-rich chondrites Queen Alexandra Range 94411 and Hammadah al Hamra 237

  摘要：

  Abstract—Fine‐grained, heavily‐hydrated lithic clasts in the metal‐rich (CB) chondrites Queen Alexandra Range (QUE) 94411 and Hammadah al Hamra 237 and CH chondrites, such as Patuxent Range (PAT) 91546 and Allan Hills (ALH) 85085, are mineralogically similar suggesting genetic relationship between these meteorites. These clasts contain no anhydrous silicates and consist of framboidal and platelet magnetite, prismatic sulfides (pentlandite and pyrrhotite), and Fe‐Mn‐Mg‐bearing Ca‐carbonates set in a phyllosilicate‐rich matrix. Two types of phyllosilicates were identified: serpentine, with basal spacing of ˜0.73 nm, and saponite, with basal spacings of about 1.1–1.2 nm. Chondrules and FeNi‐metal grains in CB and CH chondrites are believed to have formed at high temperature (>1300 K) by condensation in a solar nebula region that experienced complete vaporization. The absence of aqueous alteration of chondrules and metal grains in CB and CH chondrites indicates that the clasts experienced hydration in an asteroidal setting prior to incorporation into the CH and CB parent bodies. The hydrated clasts were either incorporated during regolith gardening or accreted together with chondrules and FeNi‐metal grains after these high‐temperature components had been transported from their hot formation region to a much colder region of the solar nebula.

  DOI：

  10.1111/j.1945-5100.2002.tb01110.x
• 作为产物：
  描述：

  顺式-3-戊烯-1-炔 在 甲醇 、 ammonium chloride 、 copper(l) chloride 作用下， 生成 deca-2c,8c-diene-4,6-diyne
  参考文献：
  名称：

  Viehe, Chemische Berichte, 1959, vol. 92, p. 3064,3071

  摘要：

  DOI：

文献信息

• Bohlmann; Sinn, Chemische Berichte, 1955, vol. 88, p. 1869,1877
  作者：Bohlmann、Sinn

  DOI：——

  日期：——
• Bell et al., Journal of the Chemical Society, 1958, p. 1313,1320
  作者：Bell et al.

  DOI：——

  日期：——
• Viehe, Chemische Berichte, 1959, vol. 92, p. 3064,3071
  作者：Viehe

  DOI：——

  日期：——
• Heavily-hydrated lithic clasts in CH chondrites and the related, metal-rich chondrites Queen Alexandra Range 94411 and Hammadah al Hamra 237
  作者：Ansgar GRESHAKE、Alexander N. KROT、Anders MEIBOM、Michael K. WEISBERG、Michael E. ZOLENSKY、Klaus KEIL

  DOI：10.1111/j.1945-5100.2002.tb01110.x

  日期：2002.2

  Abstract—Fine‐grained, heavily‐hydrated lithic clasts in the metal‐rich (CB) chondrites Queen Alexandra Range (QUE) 94411 and Hammadah al Hamra 237 and CH chondrites, such as Patuxent Range (PAT) 91546 and Allan Hills (ALH) 85085, are mineralogically similar suggesting genetic relationship between these meteorites. These clasts contain no anhydrous silicates and consist of framboidal and platelet magnetite, prismatic sulfides (pentlandite and pyrrhotite), and Fe‐Mn‐Mg‐bearing Ca‐carbonates set in a phyllosilicate‐rich matrix. Two types of phyllosilicates were identified: serpentine, with basal spacing of ˜0.73 nm, and saponite, with basal spacings of about 1.1–1.2 nm. Chondrules and FeNi‐metal grains in CB and CH chondrites are believed to have formed at high temperature (>1300 K) by condensation in a solar nebula region that experienced complete vaporization. The absence of aqueous alteration of chondrules and metal grains in CB and CH chondrites indicates that the clasts experienced hydration in an asteroidal setting prior to incorporation into the CH and CB parent bodies. The hydrated clasts were either incorporated during regolith gardening or accreted together with chondrules and FeNi‐metal grains after these high‐temperature components had been transported from their hot formation region to a much colder region of the solar nebula.