The surface of Mercury is dominated by extensive, widespread lava plains that formed early in its history. The emplacement of these lavas was accompanied by the release of magmatic volatiles, the bulk of which were lost to space via thermal escape and/or photodissociation. Here we consider the fate of these erupted volatiles by quantifying the volumes of erupted volcanic plains and estimating the associated masses of erupted volatiles. The concentrations and speciation of volatiles in Mercury's magmas are not known with certainty at this time, so we model a wide range of cases, based on existing experimental data and speciation models, at 3–7 log fO₂ units below conditions determined by the iron-wüstite buffer. Cases range from relatively low gas content scenarios (total exsolved gas mass of $9\times {10}^{15}$ kg) to high gas content scenarios (total exsolved gas = 5 × 10¹⁹ kg). We estimate that the average duration of a transient volcanic atmosphere resulting from a single eruption would be between ∼250 and ∼210,000 years, depending on the volume, degassed volatile content, and eruption rate of an individual eruption, as well as the fO₂ conditions of the planet's interior. If a dense transient atmosphere was ever surface-bound long enough for the released volatiles to be transported to and cold-trapped at Mercury's polar regions, those trapped volatiles are predicted to be well-mixed with the regolith, and at least 16 m beneath the surface given regolith gardening rates. These volatiles would have a composition and age distinctly different from those of the H₂O-ice deposits observed at the poles of Mercury today.

水星的表面以其历史早期形成的广泛而广泛的熔岩平原为主。这些熔岩的到位伴随着岩浆挥发物的释放，岩浆挥发物的大部分通过热逸出和/或光离解而损失到太空中。在这里，我们通过对火山喷发平原的数量进行量化并估算与之相关的喷发挥发物的质量，来考虑这些喷发挥发物的命运。目前尚不确定水星岩浆中挥发物的浓度和形态，因此，根据现有的实验数据和形态模型，我们在3–7 log f O ₂的情况下对各种情况进行了建模低于铁白钨缓冲液确定的条件下的单位。案例的范围从相对低的气体含量情景（总溶解气体质量为$9\times {10}^{15}$到高含气量情景（总溶解气体= 5×10 ¹⁹公斤）。我们估计，由一次喷发导致的瞬时火山大气的平均持续时间将在约250至〜210,000年之间，这取决于单个喷发的体积，脱气的挥发物含量和喷发率以及f O _2。行星内部的条件。如果稠密的瞬态大气的表面结合时间足够长，足以将释放出的挥发物转移到水星的极地并在其水冷极处捕获，则这些捕获的挥发物预计将与重灰石充分混合，并且至少在地幔下方16 m处。给定的表面灰泥园艺率。这些挥发物的组成和年龄与H的明显不同今天在水星两极观察到_2种O型冰沉积物。