Heterogeneities from the first 100 million years recorded in deep mantle noble gases from the Northern Lau Back-arc Basin

Pető, Mária; Mukhopadhyay, Sujoy; Kelley, K. A.

doi:10.1016/j.epsl.2013.02.012

Cited by 65 publications

(93 citation statements)

References 80 publications

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“…Indeed, as shown in Section 5.2 above, the composition of the peridotitic component has close to no impact on the magma composition and the lavas isotopic compositions are completed buffered by the mixed recycled component, basalt and sediment. It is also clearly the case for noble gazes, as demonstrated by Mukhopadhyay (2012) and Pető et al (2013). So maybe He is the sole tracer that keeps the memory of a potential primitive material in plume source but the processes that could explain it remain to be found.…”

Section: Gambier Fozo and The 'Railway Crossing'mentioning

confidence: 92%

Combined petrological, geochemical and isotopic modeling of a plume source: Example of Gambier Island, Pitcairn chain

Delavault

Chauvel

Sobolev

et al. 2015

Earth and Planetary Science Letters

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Section: Gambier Fozo and The 'Railway Crossing'mentioning

confidence: 92%

Combined petrological, geochemical and isotopic modeling of a plume source: Example of Gambier Island, Pitcairn chain

Delavault

Chauvel

Sobolev

et al. 2015

Earth and Planetary Science Letters

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“…By contrast, the formation age of the EarthMoon system is uncertain and is presently debated within a time interval of 30- the Earth requires the development of adequate extinct radioactivity chronometers. Because the Earth's interior has been well mixed by mantle convection over 4.5 Ga, most of the early reservoirs have been rehomogenized, even if some remnants of past heterogeneities might still be present [4][5][6][7]. However, information on ancient reservoirs is still held at the Earth's surface, in old terranes, and, in the case of noble gases, in the terrestrial atmosphere.…”

Section: Introductionmentioning

confidence: 99%

The iodine–plutonium–xenon age of the Moon–Earth system revisited

Avice

Marty

2014

Phil. Trans. R. Soc. A.

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Iodine-plutonium-xenon isotope systematics have been used to re-evaluate time constraints on the early evolution of the Earth-atmosphere system and, by inference, on the Moon-forming event. Two extinct radionuclides ( 129 I, T 1/2 = 15.6 Ma and 244 Pu, T 1/2 = 80 Ma) have produced radiogenic 129 Xe and fissiogenic 131−136 Xe, respectively, within the Earth, the related isotope fingerprints of which are seen in the compositions of mantle and atmospheric Xe. Recent studies of Archaean rocks suggest that xenon atoms have been lost from the Earth's atmosphere and isotopically fractionated during long periods of geological time, until at least the end of the Archaean eon. Here, we build a model that takes into account these results. Correction for Xe loss permits the computation of new closure ages for the Earth's atmosphere that are in agreement with those computed for mantle Xe. The corrected Xe formation interval for the Earth-atmosphere system is 40 +20 −10 Ma after the beginning of Solar System formation. This time interval may represent a lower limit for the age of the Moon-forming impact.

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“…Warren et al 1999;Walker 2009 (Fig. 2, Mukhopadhyay (2012), Pető et al (2013), Parai and Mukhopadhyay (2015), Caracausi et al (2016)). If the mantle had a homogeneous I/Pu ratio, the higher 129 * Xe/ 136 * Xe Pu ratio in the MORB source would paradoxically imply that the shallow mantle became closed to volatile loss earlier than the deep mantle.…”

Section: Volatile Sources and The History Of Volatile Deliverymentioning

confidence: 99%

“…2 Ratios of I-to Pu-derived Xe in plume source and MORB source assuming a chondritic starting composition for Xe isotopes in the mantle (Caracausi et al 2016). The plume average was compiled from data presented in Mukhopadhyay (2012), Pető et al (2013), and Caracausi et al (2016). The MORB average is from Parai and Mukhopadhyay (2015) Fig .…”

Section: Volatile Sources and The History Of Volatile Deliverymentioning

confidence: 99%

Atmosphere Impact Losses

Schlichting

Mukhopadhyay

2018

Space Sci Rev

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Determining the origin of volatiles on terrestrial planets and quantifying atmospheric loss during planet formation is crucial for understanding the history and evolution of planetary atmospheres. Using geochemical observations of noble gases and major volatiles we determine what the present day inventory of volatiles tells us about the sources, the accretion process and the early differentiation of the Earth. We further quantify the key volatile loss mechanisms and the atmospheric loss history during Earth's formation. Volatiles were accreted throughout the Earth's formation, but Earth's early accretion history was volatile poor. Although nebular Ne and possible H in the deep mantle might be a fingerprint of this early accretion, most of the mantle does not remember this signature implying that volatile loss occurred during accretion. Present day geochemistry of volatiles shows no evidence of hydrodynamic escape as the isotopic compositions of most volatiles are chondritic. This suggests that atmospheric loss generated by impacts played a major role during Earth's formation. While many of the volatiles have chondritic isotopic ratios, their relative abundances are certainly not chondritic again suggesting volatile loss tied to impacts. Geochemical evidence of atmospheric loss comes from the 3 He/ 22 Ne, halogen ratios (e.g., F/Cl) and low H/N ratios. In addition, the geochemical ratios indicate that most of the water could have been delivered prior to the Moon forming impact and that the Moon forming impact did not drive off the ocean. Given the importance of impacts in determining the volatile budget of the Earth we examine the contributions to atmospheric loss from both small and large impacts. We find that atmospheric mass loss due to impacts can be characterized into three different regimes: 1) Giant Impacts, that create a strong shock transversing the whole planet and that can lead to atmospheric loss globally. 2) Large enough impactors (m cap √ 2ρ 0 (πhR) 3/2 , r cap ∼ 25 km for the current Earth), that are able to eject all the atmosphere above the tangent plane of the impact site, where h, R and ρ 0 are the atmospheric scale height, radius of the target, and its atmospheric density at the ground. 3) Small impactors (m min > 4πρ 0 h 3 , r min ∼ 1 km for the current Earth), that are only able to eject a fraction of the atmospheric mass above the tangent plane. We demonstrate that per unit impactor mass, small impactors with r min < r < r cap are the most efficient impactors in eroding the atmosphere. In fact for the current atmospheric mass of the Earth, they are more than five orders of magnitude more efficient (per unit impactor mass) than giant impacts, implying that atmospheric mass loss must have been common. The enormous atmospheric mass loss efficiency of small impactors is due to the fact that most of their impact energy and momentum is directly available for local mass loss, where as in the giant impact regime a lot of energy and momentum is 'wasted' by having to create a strong shock th...

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Heterogeneities from the first 100 million years recorded in deep mantle noble gases from the Northern Lau Back-arc Basin

Abstract: 10Heavy noble gases (Ne, Ar, Xe) can record long-lasting heterogeneities in the mantle 11 because of the production of isotopes from extant ( 238 U, 40

Cited by 65 publications

References 80 publications

Combined petrological, geochemical and isotopic modeling of a plume source: Example of Gambier Island, Pitcairn chain

Combined petrological, geochemical and isotopic modeling of a plume source: Example of Gambier Island, Pitcairn chain

The iodine–plutonium–xenon age of the Moon–Earth system revisited

Atmosphere Impact Losses

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