Mars' atmospheric neon suggests volatile-rich primitive mantle
arXiv:2108.11537 · doi:10.1016/j.icarus.2021.114685
Abstract
Martian atmospheric neon (Ne) has been detected by Viking and also found as trapped gas in Martian meteorites, though its abundance and isotopic composition have not been well determined. Because the timescale of Ne loss via atmospheric escape estimated from recent measurements with MAVEN is short (0.6--1 10 years), the abundance and isotope composition of Martian atmospheric Ne reflect recent atmospheric gas supply mostly from volcanic degassing. Thus, it can serve as a probe for the volatile content of the interior. Here we show that the tentatively-informed atmospheric Ne abundance suggests recent active volcanism and the mantle being richer in Ne than Earth's mantle today by more than a factor of 5--80. The estimated mantle Ne abundance requires efficient solar nebular gas capture or accretion of Ne-rich materials such as solar-wind-implanted dust in the planet formation stage, both of which provide important constraints on the abundance of other volatile elements in the interior and the accretion history of Mars. More precise determination of atmospheric Ne abundance and isotopic composition by in situ analysis or Mars sample return is crucial for distinguishing the possible origins of Ne.
arXiv comment57 pages, 4 figures, accepted for publication in Icarus
References in corpus (38)
- The origins and concentrations of water, carbon, nitrogen and noble gases on Earth
- Evolution of the Solar Activity over Time and Effects on Planetary Atmospheres: I. High-energy Irradiances (1-1700 A)
- Most 1.6 Earth-Radius Planets are not Rocky
- The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
- Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
- Measured Mass Loss Rates of Solar-like Stars as a Function of Age and Activity
- The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
- Warming early Mars with CO2 and H2
- Transient reducing greenhouse warming on early Mars
- The Extreme Ultraviolet and X-Ray Sun in Time: High-Energy Evolutionary Tracks of a Solar-Like Star
- Constraints on the mass of a habitable planet with water of nebular origin
- Hydrodynamics of Embedded Planets' First Atmospheres. II. A Rapid Recycling of Atmospheric Gas
- Evidence for multiple magma ocean outgassing and atmospheric loss episodes from mantle noble gases
- The Dual Origin of the Terrestrial Atmosphere
- Origin of the Ocean on the Earth: Early Evolution of Water D/H in a Hydrogen-rich Atmosphere
- Tracing the fate of carbon and the atmospheric evolution of Mars
- Grain size constraints on HL Tau with polarization signature
- Evolution of Water Reservoirs on Mars: Constraints from Hydrogen Isotopes in Martian Meteorites
- The efficiency of dust trapping in ringed proto-planetary discs
- Estimate on dust scale height from ALMA dust continuum image of the HD 163296 protoplanetary disk
- Suppression of atmospheric recycling of planets embedded in a protoplanetary disc by buoyancy barrier
- A warmer and wetter solution for early Mars and the challenges with transient warming
- Evidence for geologically recent explosive volcanism in Elysium Planitia, Mars
- Krypton isotopes and noble gas abundances in the coma of comet 67P/Churyumov-Gerasimenko
- Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
- A Lower Limit of Atmospheric Pressure on Early Mars Inferred from Nitrogen and Argon Isotopic Compositions
- Loss and fractionation of noble gas isotopes and moderately volatile elements from planetary embryos and early Venus, Earth and Mars
- Radial variations in grain sizes and dust scale heights in the protoplanetary disk around HD 163296 revealed by ALMA polarization observation
- Small Planetesimals in a Massive Disk Formed Mars
- On the filtering and processing of dust by planetesimals 1. Derivation of collision probabilities for non-drifting planetesimals
- Scattering-induced intensity reduction: large mass content with small grains in the inner region of the TW Hya disk
- Anoxic Atmospheres on Mars Driven by Volcanism: Implications for Past Environments and Life
- Delivery of organics to Mars through asteroid and comet impacts
- Gas flow around a planet embedded in a protoplanetary disc: the dependence on the planetary mass
- Impact degassing and atmospheric erosion on Venus, Earth, and Mars during the late accretion
- Influences of three-dimensional gas flow induced by protoplanets on pebble accretion --. shear regime
- Influences of protoplanet-induced three-dimensional gas flow on pebble accretion . Headwind regime
- The Dynamic Proto-atmospheres around Low-Mass Planets with Eccentric Orbits