Recent studies have detected structurally bound water in the refractory silicate minerals present in ordinary and enstatite chondrite meteorites. The mechanism for the incorporation of the hydrogen is not well defined. In this paper we quantitatively examine a two-fold process involving the implantation and diffusion of nebular hydrogen ions that is responsible for the hydration of the chondritic minerals. Our simulations show that depending on critical parameters, including the flux of the protons in nebular plasma, retention coefficient, temperature of the silicate minerals, and desorption rate of implanted hydrogen, the implantation of low-energy hydrogen ions can result in equivalent water contents of ∼0.1 wt% in chondritic silicates within 10 years. Thus, this novel mechanism operating in the nebula at 10⁻³ bar pressure and <650 K temperatures can efficiently hydrate the free-floating chondritic minerals prior to the rapid formation of planetesimals inside the snow line, and agree well with the wet accretion scenario for the inner solar system objects.

最近的研究已经在普通和顽火球粒陨石中存在的难熔硅酸盐矿物中检测到结构结合水。掺入氢的机制尚不明确。在本文中，我们定量研究了一个双重过程，该过程涉及负责球粒陨石矿物水合的星云氢离子的注入和扩散。我们的模拟表明，根据关键参数，包括星云等离子体中质子的通量、保留系数、硅酸盐矿物的温度和注入氢的解吸率，低能氢离子的注入可以导致等效的水含量在 10 年内在球粒状硅酸盐中约 0.1 wt%。因此，这种新颖的机制在 10 ^-3的星云中运行 bar 压力和 <650 K 温度可以在雪线内快速形成小行星之前有效地水合自由漂浮的球粒陨石矿物，并且与内部太阳系物体的湿吸积情景非常吻合。