Lutz B L, Owen T, De Bergh C
Lowell Observatory, Flagstaff, Arizona 86001, USA.
Icarus. 1990;86:329-35. doi: 10.1016/0019-1035(90)90223-v.
We have estimated the D/H ratio that may have been present in the primitive ices in the protosolar nebula. Using observations of the CH3D/CH4 ratio in the outer planets, we developed two simple but limiting models which constrain the amount of dilution that deuterated volatiles which were contributed to the planetary atmospheres by evaporated primordial ices may have undergone by mixing with the original hydrogen envelopes. The models suggest that the D/H ratio in these ices was probably somewhere between a few times 10(-4) and 10(-3). These planetary-atmosphere-derived results are compared with other solar system bodies thought to contain primitive material and with D/H ratios observed in interstellar polyatomic molecules.
我们估算了原太阳星云原始冰体中可能存在的D/H比率。利用对外行星中CH3D/CH4比率的观测，我们建立了两个简单但具有局限性的模型，这些模型限制了由蒸发的原始冰体贡献给行星大气的氘化挥发物通过与原始氢包层混合可能经历的稀释量。模型表明，这些冰体中的D/H比率可能在10的负4次方的几倍到10的负3次方之间。将这些源自行星大气的结果与其他被认为含有原始物质的太阳系天体以及在星际多原子分子中观测到的D/H比率进行了比较。
