What distinctive geological features on Mercury are thought to be direct evidence of ongoing volatile processes beneath the surface?
Answer
Hollows
Hollows are identified as shallow, irregular depressions that serve as compelling visual proof of current volatile activity on Mercury. The prevailing mechanism suggests that volatile compounds, such as sulfur-bearing compounds buried underneath, undergo sublimation, transitioning directly into a gaseous state. This process creates empty voids within the subsurface structure. When the crust overlying these voids can no longer support its own weight, it collapses downward, resulting in the characteristic morphology observed as hollows. Their active presence implies that substantial reservoirs of these volatiles persist within the planet's interior, surviving the intense external heat.
Related Questions
Which volatile elements did the MESSENGER mission confirm are present in surprisingly high quantities on Mercury's surface and crust?What distinctive geological features on Mercury are thought to be direct evidence of ongoing volatile processes beneath the surface?What implication does the detection of chlorine, sulfur, and potassium have on the prior classification of Mercury's bulk composition?According to the comparison table, which category of elements challenges the simplest high-heat formation models due to their observed abundance on Mercury?Which specific formation theory suggests Mercury acquired its volatile-rich components via a 'late veneer' after the inner solar system's high-heat phase?What specific implication does the detection of chlorine suggest regarding the condensation temperatures during Mercury's early history?How does the process of Crustal Sequestration account for retaining volatiles despite the high heat required for Mercury's core differentiation?What chemical characteristic of the material forming Mercury's mantle supports the idea that source material contained substantial volatiles?What alternative scenario is suggested if Mercury formed *in situ* from standard solar nebula material at 0.3 to 0.4 AU, contrary to observations?What mechanism related to rapid formation could potentially explain Mercury retaining volatiles near the Sun, according to formation implications?What broader scientific importance does understanding Mercury's volatile retention hold for inner solar system formation studies?