Presentation on theme: "The Late Veneer: constraints on composition, mass, and mixing timescales “Post-AGU” Divya Allupeddinti Beth-Ann Bell Lea Bello Ana Cernok Nilotpal Ghosh."— Presentation transcript:
The Late Veneer: constraints on composition, mass, and mixing timescales “Post-AGU” Divya Allupeddinti Beth-Ann Bell Lea Bello Ana Cernok Nilotpal Ghosh Peter Olds Clemens Prescher Jonathan Tucker Matt Wielicki Kevin Zahnle Michael Manga
Late veneer is mixed by 2.9 Ga Maier et al., 2009
Questions and Hypotheses What kind of impactors were they? – Constraints from geochemistry, size-frequency distributions – Determines number, size, density of impactors How efficiently does the mantle homogenize? – Determines the mixing timescale of the mantle under different delivery regimes – Populate a possible parameter space
Constraints from Geochemistry We take a new look at PGE abundances and tungsten isotope systematics to constrain the mass of the late veneer. We use radiogenic osmium isotope systematics to put constraints on the compositions of the impactor(s). 190 Pt- 186 Os system 187 Re- 187 Os system We tried to use other, stable isotope systems to put constraints on the composition of the impactors. But nothing works as well as the PGE, W, and Os isotopes.
PGE Abundances % of BSE mass% Impactor PopulationReOsIrRuPtPd Average for population stdev for population c. chondrites0.650.580.550.780.651.090.720.20 e. chondrites0.600.580.570.760.610.790.650.10 ordinary chondrites0.530.51 0.680.550.940.620.17 Average for element0.590.560.550.740.600.94 stdev for element0.060.040.030.05 0.15 Assumes zero PGE in the earth’s mantle after core formation. ~0.6% addition required (if chondritic). Tungsten isotopes provide an independent constraint. Returns the same mass for the late veneer.
Osmium Isotopes This shows the present-day mixing line. But we also need to account for radiogenic ingrowth over time. 187 Re 187 Os, t 1/2 ~ 42 Ga 190 Pt 186 Os, t 1/2 ~ 650 Ga Meteorite data: Brandon et al. (2005)
Some Uncertainties: a) the initial 186 Os/ 188 Os and 187 Os/ 188 Os values. b) effects of Re mobility on the Re/Os ratios. Assumes closed-system, radiogenic ingrowth only Goal: composition/timing solutions that reasonably re-create Earth’s osmium
Constraints of Impact Flux (ancient-SFD) Collisional evolution model provides constraints on the size-frequency distribution of the asteroid belt We take 200km impactors as the largest due to SPA crater >95% of the mass is delivered by >50km impactors (Bottke et al., 2005) Diameter (km) Bottke 2010 ancient Number Diameter (m)Radius (m)Density (Kg.m^3)Mass (Kg)%mass delivered 120000010000027001.13E+1957.8 51000005000027007.07E+1836.1 6.666665500002500027001.18E+186.0 7.510000500027001.06E+160.1 10100050027001.41E+130.0 Total Mass (Kg)1.96E+19100.0
Bottke 2010 Today NumberDiameter (m)Radius (m)Density (Kg.m^3)Mass (Kg)%mass delivered 120000010000027001.13E+1937 101000005000027001.41E+1946 30500002500027005.30E+1817 60000100050027008.48E+160 Total Mass (Kg)3.08E+19100 Constraints of Impact Flux (present-SFD) Size-frequency distribution of present-day main asteroid belt We take 200km impactors as the largest due to SPA crater >95% of the mass is delivered by >50km impactors (Bottke et al., 2005) Diameter (km)
Endmember scenario(many small impactors) “(1) a residual population of small planetesimals containing 0.01 M ⊕ is able to damp the high eccentricities and inclinations of the terrestrial planets after giant impacts to their observed values. (2) At the same time, this planetesimal population can account for the observed relative amounts of late veneer added to the Earth, Moon and Mars provided that the majority of the accreted late veneer was delivered by small planetesimals with radii <10 m.”
Endmember scenario (single impactor) Depending on density our calculations suggest that you would need an impactor of ~2500km to provide the mass necessary for the late-veneer Lunar HSE abundances are >20 times lower than Earth and Mars (could mean that relying on the lunar record is not sufficient) (Bottke et al., 2010) NumberDiameter (m)Radius (m)Density (Kg.m^3)Mass (Kg) 12050000102500054002.44E+22 12410000120500033002.42E+22 12500000125000030002.45E+22 12600000130000027002.48E+22 9452500026250034202.44E+22 (4 Vesta, Dawn Mission Image)
Mass delivered during LHB Mass delivered to Moon during LHB (including SPA) is 2.22 x 10 19 kg Scaled to the Earth’s ~20-30x gravitational cross-section, total mass delivery to the Earth of 4-6 x 10 20 kg of material or 1.9-2.8% of the total estimated for the late-veneer If we account for the Moons deficiency of HSE we account for 35-55% of the abundance of HSE delivered to the Earth during the LHB suggesting at least one and maybe two LHB- style events prior to ~3.8 Ga LHB CraterNumber Crater diameter (m) Impactor diameter (m)Radius (m) Density (Kg.m^3)Mass (Kg) %mass delivered SPA1224000022400011200027001.59E+1971.4 Nectaris1860000860004300027008.99E+174.0 Imbrium111600001160005800027002.21E+189.9 Orientale1930000930004650027001.14E+185.1 Crisium110600001060005300027001.68E+187.6 Serenitatis1674000674003370027004.33E+171.9 Total Mass (Kg)2.22E+19100.0 (Zahnle et al., 2007)
Dynamic Approach 2-D (Citcom) & 3-D (StagYY) spherical convection models Crater anomalies introduced into a convecting mantle Three possible scenarios to account for isotopic compositions 1.A distribution of small sized impactors 2.A size-frequency distribution estimated from lunar cratering record 3.A single large impactor
Preliminary Conclusions, Future Work We are able to reproduce mass estimates for the late veneer and have tried to use osmium isotopes to put constraints on the composition and timing of the late veneer. Majority of the mass is delivered with large (>50 km) projectiles assuming an asteroidal SFD. Up to 35-55% of the late-veneer mass was added during the LHB suggesting at least one if not two LHB events prior ~3.8 Ga Mixing timescales are on the order of magnitude suggested from komatiites and appears to be independent of Ra however highly dependent on Q. Future Work: Scaling laws for impactor material deposition within impact craters, allow communication with the core when PGE material is at CMB, account for new estimates of high rotation rates and oblateness, deliver PGE in some modeled time steps, and…….