Noble gases in CM carbonaceous chondrites: Effect of parent body aqueous and thermal alteration and cosmic ray exposure ages

Krietsch, Daniela; Busemann, H.; Riebe, M. E. I.; King, A. J.; Alexander, Conel M. O'd.; Maden, C.

doi:10.1016/j.gca.2021.05.050

Cited by 33 publications

(37 citation statements)

References 112 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For argon, 38 Ar/ 36 Ar ratios are compatible with either the atmospheric 38 Ar/ 36 Ar ratio (≈0.188; Ozima and Podosek, 2002) or the 38 Ar/ 36 Ar ratio of argon in phase Q (≈0.187; Ott, 2002). However, the 40 Ar/ 36 Ar ratios range from 3 to 43, well below the atmospheric value (≈300, Ozima and Podosek, 2002), but typical for trapped argon contained in carbonaceous chondrites (Krietsch et al, 2021). The isotopic ratios of Kr and Xe are distinct from those of air, as well, and are similar again, to those measured for bulk carbonaceous chondrites (e.g., Krietsch et al, 2021).…”

Section: Results Of Noble Gas Measurements and Cosmic-ray Exposure Agesmentioning

confidence: 80%

“…However, the 40 Ar/ 36 Ar ratios range from 3 to 43, well below the atmospheric value (≈300, Ozima and Podosek, 2002), but typical for trapped argon contained in carbonaceous chondrites (Krietsch et al, 2021). The isotopic ratios of Kr and Xe are distinct from those of air, as well, and are similar again, to those measured for bulk carbonaceous chondrites (e.g., Krietsch et al, 2021). The first heating steps of Tarda and Tagish Lake samples reveal the presence of weakly bound atmospheric gases (Fig.…”

Section: Results Of Noble Gas Measurements and Cosmic-ray Exposure Agesmentioning

confidence: 95%

“…In the three isotope diagram, the neon isotopic compositions of bulk chondrites plot within a space defined by cosmogenic Ne, Ne-Q and a pole with ( 20 Ne/ 22 Ne) slightly below that of Ne-HL carried by presolar nanodiamonds (Fig. 1; Huss and Lewis, 1994;Krietsch et al, 2021). The latter is likely due to the presence of Ne-E from presolar SiC or graphite (Riebe et al, 2020).…”

Section: Discussionmentioning

confidence: 96%

See 2 more Smart Citations

Origin of radiogenic 129Xe variations in carbonaceous chondrites

Avice¹,

Meier²,

Marrocchi³

2022

Geochem. Persp. Let.

View full text Add to dashboard Cite

Carbonaceous chondrites are pristine witnesses of the formation of the solar system. Among them, the carbon-rich Tarda and Tagish Lake meteorites are thought to have sampled very distant regions of the outer circumsolar disk (Hiroi et al., 2001). Here, we show that their noble gas isotopic compositions (especially 129 Xe excesses) are similar, implying their formation in comparable environments. Combined with literature data, we show that the radiogenic excesses of 129 Xe relative to solar wind in carbonaceous chondrites define anti-correlations with their respective iodine and carbon contents. These trends do not result from the heterogeneous distribution of 129 I in the disk but rather evidence a xenon dilution effect; the radiogenic 129 Xe excesses being dominated by trapped xenon in the most carbon-rich carbonaceous chondrites. Our data also suggest that both Tarda and Tagish Lake accreted beyond 10 astronomical units, in regions of the disk that were cold enough for CO 2 to condense.

show abstract

Section: Results Of Noble Gas Measurements and Cosmic-ray Exposure Agesmentioning

confidence: 80%

Section: Results Of Noble Gas Measurements and Cosmic-ray Exposure Agesmentioning

confidence: 95%

Section: Discussionmentioning

confidence: 96%

See 1 more Smart Citation

Origin of radiogenic 129Xe variations in carbonaceous chondrites

Avice¹,

Meier²,

Marrocchi³

2022

Geochem. Persp. Let.

View full text Add to dashboard Cite

show abstract

“…The only available measures of the helium isotope ratio are based on terrestrial and solar system environments, including the Earth's mantle ( 3 He/ 4 He = [1.1-4.2] × 10 −5 ; Péron et al 2018), meteorites ( 3 He/ 4 He = [1. ] × 10 −4 ; Busemann et al 2000;Krietsch et al 2021), the Local Interstellar Cloud ( 3 He/ 4 He = 1.62 ± 0.29 × 10 −4 ; Busemann et al 2006), Jupiter ( 3 He/ 4 He = 1.66 ± 0.05 × 10 −4 ; Mahaffy et al 1998), and solar wind particles ( 3 He/ 4 He = [4.5-4.8] × 10 −4 ; Heber et al 2012). The elevated values measured from the present-day solar wind reflect the burning of deuterium into 3 He during the pre-main-sequence evolution of the Sun.…”

Section: Introductionmentioning

confidence: 99%

Primordial Helium-3 Redux: The Helium Isotope Ratio of the Orion Nebula*

Cooke

Noterdaeme

Johnson

et al. 2022

ApJ

View full text Add to dashboard Cite

We report the first direct measurement of the helium isotope ratio, 3He/4He, outside of the Local Interstellar Cloud, as part of science-verification observations with the upgraded CRyogenic InfraRed Echelle Spectrograph. Our determination of 3He/4He is based on metastable He i* absorption along the line of sight toward Θ2A Ori in the Orion Nebula. We measure a value 3He/4He = (1.77 ± 0.13) × 10−4, which is just ∼40% above the primordial relative abundance of these isotopes, assuming the Standard Model of particle physics and cosmology, (3He/4He)p = (1.257 ± 0.017) × 10−4. We calculate a suite of galactic chemical evolution simulations to study the Galactic build up of these isotopes, using the yields from Limongi & Chieffi for stars in the mass range M = 8–100 M ⊙ and Lagarde et al. for M = 0.8–8 M ⊙. We find that these simulations simultaneously reproduce the Orion and protosolar 3He/4He values if the calculations are initialized with a primordial ratio 3 He / 4 He p = ( 1.043 ± 0.089 ) × 10 − 4 . Even though the quoted error does not include the model uncertainty, this determination agrees with the Standard Model value to within ∼2σ. We also use the present-day Galactic abundance of deuterium (D/H), helium (He/H), and 3He/4He to infer an empirical limit on the primordial 3He abundance, 3 He / H p ≤ ( 1.09 ± 0.18 ) × 10 − 5 , which also agrees with the Standard Model value. We point out that it is becoming increasingly difficult to explain the discrepant primordial 7Li/H abundance with nonstandard physics, without breaking the remarkable simultaneous agreement of three primordial element ratios (D/H, 4He/H, and 3He/4He) with the Standard Model values.

show abstract

“…The only available measures of the helium isotope ratio are based on terrestrial and Solar System environments, including the Earth's mantle ( 3 He/ 4 He = [1.1 − 4.2] × 10 −5 ; Péron et al 2018), meteorites ( 3 He/ 4 He = [1.47 − 190] × 10 −4 ; Busemann et al 2000;Krietsch et al 2021), the Local Interstellar Cloud ( 3 He/ 4 He = 1.62 ± 0.29 × 10 −4 ; Busemann et al 2006), Jupiter ( 3 He/ 4 He = 1.66 ± 0.05 × 10 −4 ; Mahaffy et al 1998), and solar wind particles ( 3 He/ 4 He = [4.5 − 4.8] × 10 −4 ; Heber et al 2012). The elevated values measured from the present day solar wind reflect the burning of deuterium into 3 He during the pre-main-sequence evolution of the Sun.…”

Section: Introductionmentioning

confidence: 99%

Primordial helium-3 redux: The helium isotope ratio of the Orion nebula

Cooke,

Noterdaeme,

Johnson

et al. 2022

Preprint

View full text Add to dashboard Cite

We report the first direct measurement of the helium isotope ratio, 3 He/ 4 He, outside of the Local Interstellar Cloud, as part of science verification observations with the upgraded CRyogenic InfraRed Echelle Spectrograph (CRIRES). Our determination of 3 He/ 4 He is based on metastable He i* absorption along the line-of-sight towards Θ 2 A Ori in the Orion Nebula. We measure a value 3 He/ 4 He = (1.77 ± 0.13) × 10 −4 , which is just ∼ 40 per cent above the primordial relative abundance of these isotopes, assuming the Standard Model of particle physics and cosmology, ( 3 He/ 4 He) p = (1.257 ± 0.017) × 10 −4 . We calculate a suite of galactic chemical evolution simulations to study the Galactic build up of these isotopes, using the yields from Limongi & Chieffi (2018) for stars in the mass range M = 8 − 100 M and Lagarde et al. (2011, 2012) for M = 0.8 − 8 M . We find that these simulations simultaneously reproduce the Orion and protosolar 3 He/ 4 He values if the calculations are initialized with a primordial ratio ( 3 He/ 4 He) p = (1.043 ± 0.089) × 10 −4 . Even though the quoted error does not include the model uncertainty, this determination agrees with the Standard Model value to within ∼ 2σ. We also use the present-day Galactic abundance of deuterium (D/H), helium (He/H), and 3 He/ 4 He to infer an empirical limit on the primordial 3 He abundance, ( 3 He/H) p ≤ (1.09 ± 0.18) × 10 −5 , which also agrees with the Standard Model value. We point out that it is becoming increasingly difficult to explain the discrepant primordial 7 Li/H abundance with non-standard physics, without breaking the remarkable simultaneous agreement of three primordial element ratios (D/H, 4 He/H, and 3 He/ 4 He) with the Standard Model values. * Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme(s) 107. 22U1.001, 194.C-0833.

show abstract

Noble gases in CM carbonaceous chondrites: Effect of parent body aqueous and thermal alteration and cosmic ray exposure ages

Cited by 33 publications

References 112 publications

Origin of radiogenic 129Xe variations in carbonaceous chondrites

Origin of radiogenic 129Xe variations in carbonaceous chondrites

Primordial Helium-3 Redux: The Helium Isotope Ratio of the Orion Nebula*

Primordial helium-3 redux: The helium isotope ratio of the Orion nebula

Contact Info

Product

Resources

About