USGS-NoGaDat - A global dataset of noble gas concentrations and their isotopic ratios in volcanic systems

ABSTRACT The abundances of the heavy elements and isotopic ratios in the present atmospheres of the giant planets can be used to trace the composition of volatiles that were present in the icy solid material that contributed to their formation. The first definitive measurements of noble gas abundances and isotope ratios at comet 67P/Churyumov–Gerasimenko (67P/C–G) were recently published by Marty et al. (2017) and Rubin et al. (2018, 2019). The implications of these abundances for the formation conditions of the 67P/C–G building blocks were then evaluated by Mousis et al. (2018a). We add here an analysis of the implications of these results for understanding the formation conditions of the building blocks of the Ice Giants and discuss how future measurements of Ice Giant atmospheric composition can be interpreted. We first evaluate the best approach for comparing comet observations with giant planet composition, and then determine what would be the current composition of the Ice Giant atmospheres based on four potential sources for their building blocks. We provide four scenarios for the origin of the Ice Giants building blocks based on four primary constraints for building block composition: (1) the bulk abundance of carbon relative to nitrogen, (2) noble gas abundances relative to carbon and nitrogen, (3) abundance ratios Kr/Ar and Xe/Ar, and (4) Xe isotopic ratios. In situ measurements of these quantities by a Galileo-like entry probe in the atmosphere(s) of Uranus and/or Neptune should place important constraints on the formation conditions of the Ice Giants.

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Noble Gases: A Record of Earth's Evolution and Mantle Dynamics

Annual Review of Earth and Planetary Sciences ◽

10.1146/annurev-earth-053018-060238 ◽

2019 ◽

Vol 47 (1) ◽

pp. 389-419 ◽

Cited By ~ 18

Author(s):

Sujoy Mukhopadhyay ◽

Rita Parai

Keyword(s):

Noble Gases ◽

Noble Gas ◽

Isotopic Ratios ◽

Mantle Structure ◽

Mantle Dynamics ◽

Mid Ocean Ridge ◽

Giant Impacts ◽

Ocean Ridge ◽

Helium Neon

Noble gases have played a key role in our understanding of the origin of Earth's volatiles, mantle structure, and long-term degassing of the mantle. Here we synthesize new insights into these topics gained from high-precision noble gas data. Our analysis reveals new constraints on the origin of the terrestrial atmosphere, the presence of nebular neon but chondritic krypton and xenon in the mantle, and a memory of multiple giant impacts during accretion. Furthermore, the reservoir supplying primordial noble gases to plumes appears to be distinct from the mid-ocean ridge basalt (MORB) reservoir since at least 4.45 Ga. While differences between the MORB mantle and plume mantle cannot be explained solely by recycling of atmospheric volatiles, injection and incorporation of atmospheric-derived noble gases into both mantle reservoirs occurred over Earth history. In the MORB mantle, the atmospheric-derived noble gases are observed to be heterogeneously distributed, reflecting inefficient mixing even within the vigorously convecting MORB mantle. ▪ Primordial noble gases in the atmosphere were largely derived from planetesimals delivered after the Moon-forming giant impact. ▪ Heterogeneities dating back to Earth's accretion are preserved in the present-day mantle. ▪ Mid-ocean ridge basalts and plume xenon isotopic ratios cannot be related by differential degassing or differential incorporation of recycled atmospheric volatiles. ▪ Differences in mid-ocean ridge basalts and plume radiogenic helium, neon, and argon ratios can be explained through the lens of differential long-term degassing.

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Noble gas monitoring at the seemingly inactive Ciomadul volcano, Eastern Carpathians, Romania

10.5194/egusphere-egu2020-869 ◽

2020 ◽

Author(s):

Boglarka-Mercedesz Kis ◽

Szabolcs Harangi ◽

László Palcsu ◽

Botond Hegyeli

Keyword(s):

Central Europe ◽

Carbon Dioxide Emissions ◽

Noble Gas ◽

Isotopic Ratios ◽

Volcanic Area ◽

Gas Emissions ◽

East Central Europe ◽

Development Fund ◽

Quaternary Volcanism ◽

Eastern Carpathians

The Ciomadul volcano is the youngest volcano (32 ka) built by the Neogene volcanism in the Carpathian-Pannonian Region. This volcanic area is characterized by intense gas emissions (Kis et al., 2017) (CO2, CH4, H2S) in the form of bubbling pools, mofettes and mineral water springs. The isotopic compositions of carbon, 13CCO2 up to -3&#8240; VPDB and helium up to 3.1 Ra suggest magmatic origin of the gas up to 80% (Kis et al., 2019).Although the volcano seems to be inactive, several features, petrologic and geophysical studies suggest that melt-bearing magmatic body could still exist beneath the volcano (Harangi et al., 2015). Moreover the geodynamic system is characterized by frequent earthquakes with magnitude up to 7 at Vrancea area, close to the CO2-rich gas emissions of Ciomadul and the neighbouring areas.In 2015 we started the monitoring of the helium isotopic ratios of Ciomadul to chech the possible relationship with seismicity. Our results show that in several cases the helium isotopic ratios increase at a seismic event with magnitude between 4 and 5.8 suggesting a relationship between the two phenomena.&#160;Harangi, Sz., Luk&#225;cs, R., Schmitt, A.K., Dunkl, I., Moln&#225;r, K., Kiss, B., Seghedi, I., &#193;. Novothny, Moln&#225;r, M. 2015, Constraints on the timing of Quaternary volcanism and duration of magma residence at Ciomadul volcano, east-central Europe, from combined U-Th/He and U-Th zircon geochronology, Journal of Volcanology and Geothermal Research, 301, 66-80Kis, B.M., Ionescu, A., Cardellini, C., Harangi, Sz., Baciu, C., Caracausi, A; Viveiros, F. 2017, Quantification of carbon dioxide emissions of Ciomadul, the youngest volcano of the Carpathian-Pannonian Region (Eastern-Central Europe, Romania), Journal of Volcanology and Geothermal Research, 341, 119&#8211;130Kis, B.M., Caracausi, A., Palcsu, L., Baciu, C., Ionescu, A., Fut&#243;, I., Sciarra, A., Harangi, Sz. 2019, Noble gas and carbon isotope systematic at the seemingly inactive Ciomadul volcano (Eastern-Central Europe, Romania, Geochemistry, Geophysics, Geosystems, 20, 6, 3019&#8211;3043This research belongs to the scientific project supported by the OTKA, K116528 (Hungarian National Research Fund), the EU and Hungary, co-&#64257;nanced by the European Regional Development Fund in the project GINOP-2.3.2-15-2016-00009 &#8216;ICER&#8217; and the Deep Carbon Observatory.

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Noble gas isotopic ratios from historical lavas and fumaroles at Mount Vesuvius (southern Italy): constraints for current and future volcanic activity

Earth and Planetary Science Letters ◽

10.1016/s0012-821x(98)00167-8 ◽

1998 ◽

Vol 164 (1-2) ◽

pp. 61-78 ◽

Cited By ~ 15

Author(s):

Dario Tedesco ◽

Keisuke Nagao ◽

Paolo Scarsi

Keyword(s):

Volcanic Activity ◽

Southern Italy ◽

Noble Gas ◽

Isotopic Ratios

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Presolar Graphite: Noble Gases and their Origins

Publications of the Astronomical Society of Australia ◽

10.1071/as03044 ◽

2003 ◽

Vol 20 (4) ◽

pp. 378-381 ◽

Cited By ~ 3

Author(s):

Sachiko Amari

Keyword(s):

Noble Gases ◽

Noble Gas ◽

Asymptotic Giant Branch ◽

Isotopic Ratios ◽

Asymptotic Giant Branch Stars ◽

Dominant Source ◽

Low Metallicity ◽

Low Mass ◽

Giant Branch Stars

AbstractPresolar graphite contains a 22Ne-rich component called Ne-E(L). Noble gas studies on graphite aggregates and single grains have shown that although a dominant source of the 22Ne is 22Na, 22Ne in the He-shell of asymptotic giant branch stars have also contributed to the Ne-E(L). In addition to novae that have been considered to be a possible source of 22Na, supernovae are a likely source as well. Krypton isotopic ratios of the separates indicate that part of graphite formed in low-mass (≤3 M⊙) asymptotic giant branch stars of low metallicity (Z ≤ 0.006).

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Science Payload for Ice Giant Entry Probes

10.5194/egusphere-egu2020-2410 ◽

2020 ◽

Cited By ~ 1

Author(s):

David H. Atkinson ◽

Olivier Mousis ◽

Thomas R. Spilker

Keyword(s):

Noble Gas ◽

Thermal Structure ◽

Acoustic Properties ◽

Isotopic Ratios ◽

Tier 2 ◽

Atmospheric Structure ◽

Structure Dynamics ◽

Tier 1 ◽

Entry Probe ◽

Probe Mission

To discern the origin and evolution of the solar system including the formation of the terrestrial planets, an understanding of giant planet formation and evolution is needed. Among the most important measurements are the atmospheric composition, structure, and processes of the ice giant. Noble gas abundances in particular are diagnostic of the conditions under which the giant planets formed, and the abundances of cloud-forming (condensable) species are indicators of both the characteristics of the protosolar nebula at the time and location of planetary formation as well as the mechanisms by which additional heavy elements might have been delivered to the planets. Although many key properties of ice giant systems can be accessed by remote observations from flyby and orbiting spacecraft, measurements of the abundances of the noble gas and key isotopes as well as deeper thermal structure, dynamics, clouds, and other atmospheric processes require direct in situ exploration by an atmospheric entry probe. Entry probe measurements can be classified as either Tier 1 or Tier 2. Tier 1 represents the minimum, threshold science required to justify the probe mission. Tier 2 is high value science that would complement and enhance the Tier 1 measurements, but alone are not enough to justify the entry probe mission. Tier 1 measurements include atmospheric abundances of noble gases (including helium), key noble gas isotope ratios 22Ne/20Ne, 36Ar/38Ar, 129Xe/total Xe, 131Xe/total Xe, and 132Xe/total Xe, additional key isotopic ratios D/H, 3He/4He, and 15N/14N, and the atmospheric thermal structure along the probe descent trajectory. To achieve the Tier 1 measurements, the probe payload must include a mass spectrometer, a helium abundance detector, and an atmospheric structure instrument including pressure and temperature sensors and an atmospheric acoustic properties sensor for speed of sound measurements from which the ratio of ortho- to para- molecular hydrogen can be determined. Depending on mission architecture and probe-carrier telecom design, Tier 1 science can be achieved with a relatively shallow probe descending to several bars. Tier 2 science includes additional key isotopic ratios such as 13C/12C and 18O/17O/16O, abundance of condensables, and additional atmospheric structure and processes including the dynamics of the atmosphere (winds and waves), the net balance of upwelling thermal infrared and downwelling solar visible radiative fluxes, and the location, structure, composition and properties of the clouds. The presence of the disequilibrium species such as PH3, CO, AsH3, GeH4, and SiH4 is primarily due to atmospheric convective upwelling, and abundance measurements would help constrain both the composition of the very deep atmosphere and deep atmosphere chemistries. Additional instrumentation necessary to fully achieve the Tier 2 objectives includes a net flux radiometer, a Nephelometer, and an ultrastable oscillator (USO) as part of the telecommunications system to enable probe Doppler tracking for measurements of atmospheric dynamics. To address all the Tier 1 and Tier 2 science objectives, a deep probe to 10 bars and beyond would provide measurements of atmospheric thermal structure, dynamics, and processes at levels beyond the direct influence of sunlight that are out of reach of remote sensing.

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