Magma Generation on Mars: Amounts, Rates, and Comparisons with Earth, Moon, and Venus

@article{Greeley1991MagmaGO,
  title={Magma Generation on Mars: Amounts, Rates, and Comparisons with Earth, Moon, and Venus},
  author={Ronald Greeley and Byron D. Schneid},
  journal={Science},
  year={1991},
  volume={254},
  pages={996 - 998}
}
Total extrusive and intrusive magma generated on Mars over the last ∼3.8 billion years is estimated at 654 x 106 cubic kilometers, or 0.17 cubic kilometers per year (km3/yr), substantially less than rates for Earth (26 to 34 km3/yr) and Venus (less than 20 km3/yr) but much more than for the Moon (0.025 km3/yr). When scaled to Earth's mass the martian rate is much smaller than that for Earth or Venus and slightly smaller than for the Moon. 

Topics from this paper

Magma generation on Mars constrained from an 40Ar degassing model
The degassing history of 40Ar on Mars is reconstructed from a model based on the Martian volcanic record. Accumulation history of 40Ar is influenced by the volcanic eruption rate at each Martian
Constraints on the depth of magnetized crust on Mars from impact craters
Large (diameter greater than ∼500 km) Martian impact basins are associated with observed magnetic fields which are statistically distinct from, and smaller than, fields associated with smaller
Recurrence Rate and Magma Effusion Rate for the Latest Volcanism on Arsia Mons, Mars
Abstract Magmatism and volcanism have evolved the Martian lithosphere, surface, and climate throughout the history of Mars. Constraining the rates of magma generation and timing of volcanism on the
Volcanism on the Red Planet: Mars
Of all of the planets in the solar system, Mars is the most Earth-like in its geologic characteristics. Like Earth, it has been subjected to exogenic processes, such as impact cratering and erosion
A comparison of inner Solar System volcanism
The volcanic landforms, eruptive sites and longevity of activity on Mercury and the Moon contrast substantially with those of Earth, Venus and Mars. Here, I synthesize global maps of volcanic and
Geologic history of Mars
Abstract Mars accumulated and differentiated into crust, mantle and core within a few tens of millions of years of Solar System formation. Formation of Hellas, which has been adopted as the base of
Long-term volumetric eruption rates and magma budgets
[1] A global compilation of 170 time-averaged volumetric volcanic output rates (Qe) is evaluated in terms of composition and petrotectonic setting to advance the understanding of long-term rates of
The present-day atmosphere of Mars: Where does it come from?
Abstract Recent observations and missions to Mars have provided us with new insight into the past habitability of Mars and its history. At the same time they have raised many questions on the planet
Mercury, Moon, Mars
The evolution of the interior of stagnant-lid bodies is comparatively easier to model and predict with respect to the Earth's due to the absence of the large uncertainties associated with the physics
The Thermo‐Chemical Evolution of Mars With a Strongly Stratified Mantle
The present-day structure of Mars and other terrestrial planets results from billions of years of thermo-chemical evolution. It is known from geodetic data (gravity field, precession, and tides) that
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 15 REFERENCES
The volcanism of Mars
Two classes of volcanic features occur on Mars: sparsely cratered plains resembling the lunar maria and circular constructs such as shields, domes, and craters. They show a markedly nonuniform
Release of Juvenile Water on Mars: Estimated Amounts and Timing Associated with Volcanism
TLDR
The amount of water released on Mars in association with volcanism is estimated to equal a layer 46 meters deep over the entire planet, based on mapping the volcanic materials and by inferring the volatile content of the lavas.
Limits on modes of lithospheric heat transport on Venus from impact crater density
We present a formalism by which the size-frequency distribution of impact craters on Venus may be used to estimate upper bounds on the mean global rates of volcanic resurfacing and lithospheric
Rates of magma emplacement and volcanic output
This study includes a compilation of about one hundred estimates of volumetric rates of magma emplacement and volcanic output that are average rates for durations of igneous activity greater than 300
Volcanism on Mars
More than 15 years of planetary exploration of Mars have given insight into the geologic processes that have shaped its surface. The newly acquired Viking data have shown that volcanism is one of the
Venus Volcanism: Initial Analysis from Magellan Data
TLDR
Magellan images confirm that volcanism is widespread and has been fimdamentally important in the formation and evolution of the crust of Venus and reveals a number of large pancake-like domes are morphologically similar to rhyolite-dacite domes on Earth.
Some Martian volcanic features as viewed from the Viking orbiters
The plains to the south and southwest of Arsia Mons are composed of elongate lava flows, many of which appear to originate at a reentrant in the Arsia Mons edifice. Individual flows can be traced for
Mars - Paleostratigraphic restoration of buried surfaces in Tharsis montes
Volcanism in the Tharsis province of Mars occurred in several different areas and was generally continuous without large time intervals between eruptive episodes. Major lava flow units are numerous
Spectral identification of geological units on the surface of Mars related to the presence of silicates from Earth‐based near‐infrared telescopic charge‐coupled device imaging
During the September 1988 Mars opposition, the authors obtained new high spatial (100-150 km) and spectral ({Delta}{lambda}/{lambda} = 1%) resolution near-IR telescopic charge-coupled device images
Chemical composition of Martian fines
Of the 21 samples acquired for the Viking X ray fluorescence spectrometer, 17 were analyzed to high precision. Compared to typical terrestrial continental soils and lunar mare fines, the Martian
...
1
2
...