Atmospheric mass and the record of liquid water on Mars
Abstract
Widespread evidence for the action of liquid water on early Mars is generally accepted to require the presence of atmospheric greenhouse agents other than CO2. Much of this activity clusters in the late Noachian and early Hesperian (3.9-3.6 Ga), and appears to coincide with a long maximum in extrusive and explosive volcanic activity. Among other suggestions, a role for S-bearing volcanic gases has been proposed, but these and any other non-CO2 greenhouse gases or atmospheric components require a background CO2 atmosphere of several hundred mbar. Global climate models suggest that even if the surface reservoir of CO2 were much larger than today, this reservoir would be mostly trapped as CO2 ice, and only a few to tens of mbar would be in the atmosphere. Thus, at the long-term steady state, sustained warmth is difficult to achieve in the face of a fainter Sun. We suggest that episodic volcanism released the CO2 trapped as ice at the planet's surface in two ways. First, the emission of S-bearing greenhouse gases (mostly SO2) would lead to warming of a few Kelvins. Second, the deposition of volcanic ash on water and CO2 ice surfaces would push the local energy budget to favor sublimation, and would also decrease the planetary albedo and lead to additional warming. Inflation of the CO2 atmosphere has been shown in global climate models to shift the distribution of snowfall to high elevations, as opposed to a latitude-dependent distribution at low atmospheric pressure. We suggest that seasonal melting of this snow carved the valley networks and filled basin lakes. The duration of warm periods was limited by the timescale for atmospheric collapse by condensation, which is 102-103 years. Repeated inflation episodes over the duration of active volcanism led to an integrated duration of aqueous activity of 106-107 years, enough to carve the valley networks. The S-bearing gases emitted by eruptions formed sulfate minerals, initially uniformly dispersed, then remobilized and locally redeposited at low latitudes during periods of aqueous activity. As volcanic activity waned in the mid-Hesperian, fewer instances of atmospheric inflation occurred, and CO2 was trapped as high-latitude surface ice. Decreasing volcanic input and gradual atmospheric escape ultimately resulted in the remaining reservoir of CO2 observed today.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2017
- Bibcode:
- 2017AGUFM.P31F..03H
- Keywords:
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- 5405 Atmospheres;
- PLANETARY SCIENCES: SOLID SURFACE PLANETS;
- 5415 Erosion and weathering;
- PLANETARY SCIENCES: SOLID SURFACE PLANETS;
- 5416 Glaciation;
- PLANETARY SCIENCES: SOLID SURFACE PLANETS;
- 5419 Hydrology and fluvial processes;
- PLANETARY SCIENCES: SOLID SURFACE PLANETS