Lee W, Wdowiak T J
Department of Physics, The University of Alabama at Birmingham 35294-1170, USA.
Astrophys J. 1993 Nov 1;417(1):L49-51. doi: 10.1086/187091.
We report the results of an experiment that produced a residue which closely matches the hydrocarbon component of the Murchison carbonaceous chondrite. This experiment suggests that the parent material of the meteoritic component originated as polycyclic aromatic hydrocarbon species in carbon stars during their later stages of evolution. The experiments also indicate that the pathway from those formation sites to eventual incorporation into the meteorite parent body involved hydrogenation in a plasma in the solar nebula or in H II regions prior to the solar nebula. This model is consistent with what is known about the meteoritic hydrocarbon component including deuterium abundance, the observation of cosmic infrared emission bands best attributed to polycyclic aromatic hydrocarbon molecules, and the inherent stability of these molecules that allows their formation in stars and subsequent survival in the interstellar medium.
我们报告了一项实验的结果，该实验产生了一种与默奇森碳质球粒陨石的碳氢化合物成分紧密匹配的残留物。该实验表明，陨石成分的母体物质起源于碳星演化后期的多环芳烃物种。实验还表明，从那些形成地点到最终并入陨石母体的途径涉及在太阳星云或太阳星云之前的H II区域的等离子体中氢化。该模型与关于陨石碳氢化合物成分的已知信息一致，包括氘丰度、最归因于多环芳烃分子的宇宙红外发射带的观测，以及这些分子的固有稳定性，使其能够在恒星中形成并随后在星际介质中存活。
