Origin of excess 176Hf in meteorites

Research output: Contribution to journal › Journal article › Research › peer-review

Standard

Origin of excess 176Hf in meteorites. / Thrane, Kristine; Connelly, James; Bizzarro, Martin; Meyer, Bradley S.; The, Lin-Sin.

In: The Astrophysical Journal, Vol. 717, No. 2, 2010, p. 861-867.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Thrane, K, Connelly, J, Bizzarro, M, Meyer, BS & The, L-S 2010, 'Origin of excess 176Hf in meteorites', The Astrophysical Journal, vol. 717, no. 2, pp. 861-867. https://doi.org/10.1088/0004-637X/717/2/861

APA

Thrane, K., Connelly, J., Bizzarro, M., Meyer, B. S., & The, L-S. (2010). Origin of excess 176Hf in meteorites. The Astrophysical Journal, 717(2), 861-867. https://doi.org/10.1088/0004-637X/717/2/861

Vancouver

Thrane K, Connelly J, Bizzarro M, Meyer BS, The L-S. Origin of excess 176Hf in meteorites. The Astrophysical Journal. 2010;717(2):861-867. https://doi.org/10.1088/0004-637X/717/2/861

Author

Thrane, Kristine ; Connelly, James ; Bizzarro, Martin ; Meyer, Bradley S. ; The, Lin-Sin. / Origin of excess 176Hf in meteorites. In: The Astrophysical Journal. 2010 ; Vol. 717, No. 2. pp. 861-867.

Bibtex

@article{64ec12c66bce4ef8982b41356ff721c1,
title = "Origin of excess 176Hf in meteorites",
abstract = "After considerable controversy regarding the (176)Lu decay constant (lambda(176)Lu), there is now widespread agreement that (1.867 +/- 0.008) x 10(-11) yr(-1) as confirmed by various terrestrial objects and a 4557 Myr meteorite is correct. This leaves the (176)Hf excesses that are correlated with Lu/Hf elemental ratios in meteorites older than similar to 4.56 Ga meteorites unresolved. We attribute (176)Hf excess in older meteorites to an accelerated decay of (176)Lu caused by excitation of the long-lived (176)Lu ground state to a short-lived (176m)Lu isomer. The energy needed to cause this transition is ascribed to a post-crystallization spray of cosmic rays accelerated by nearby supernova(e) that occurred after 4564.5 Ma. The majority of these cosmic rays are estimated to penetrate accreted material down to 10-20 m, whereas a small fraction penetrate as deep as 100-200 m, predicting decreased excesses of (176)Hf with depth of burial at the time of the irradiation event.",
author = "Kristine Thrane and James Connelly and Martin Bizzarro and Meyer, {Bradley S.} and Lin-Sin The",
year = "2010",
doi = "10.1088/0004-637X/717/2/861",
language = "English",
volume = "717",
pages = "861--867",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing, Inc",
number = "2",

}

RIS

TY - JOUR

T1 - Origin of excess 176Hf in meteorites

AU - Thrane, Kristine

AU - Connelly, James

AU - Bizzarro, Martin

AU - Meyer, Bradley S.

AU - The, Lin-Sin

PY - 2010

Y1 - 2010

N2 - After considerable controversy regarding the (176)Lu decay constant (lambda(176)Lu), there is now widespread agreement that (1.867 +/- 0.008) x 10(-11) yr(-1) as confirmed by various terrestrial objects and a 4557 Myr meteorite is correct. This leaves the (176)Hf excesses that are correlated with Lu/Hf elemental ratios in meteorites older than similar to 4.56 Ga meteorites unresolved. We attribute (176)Hf excess in older meteorites to an accelerated decay of (176)Lu caused by excitation of the long-lived (176)Lu ground state to a short-lived (176m)Lu isomer. The energy needed to cause this transition is ascribed to a post-crystallization spray of cosmic rays accelerated by nearby supernova(e) that occurred after 4564.5 Ma. The majority of these cosmic rays are estimated to penetrate accreted material down to 10-20 m, whereas a small fraction penetrate as deep as 100-200 m, predicting decreased excesses of (176)Hf with depth of burial at the time of the irradiation event.

AB - After considerable controversy regarding the (176)Lu decay constant (lambda(176)Lu), there is now widespread agreement that (1.867 +/- 0.008) x 10(-11) yr(-1) as confirmed by various terrestrial objects and a 4557 Myr meteorite is correct. This leaves the (176)Hf excesses that are correlated with Lu/Hf elemental ratios in meteorites older than similar to 4.56 Ga meteorites unresolved. We attribute (176)Hf excess in older meteorites to an accelerated decay of (176)Lu caused by excitation of the long-lived (176)Lu ground state to a short-lived (176m)Lu isomer. The energy needed to cause this transition is ascribed to a post-crystallization spray of cosmic rays accelerated by nearby supernova(e) that occurred after 4564.5 Ma. The majority of these cosmic rays are estimated to penetrate accreted material down to 10-20 m, whereas a small fraction penetrate as deep as 100-200 m, predicting decreased excesses of (176)Hf with depth of burial at the time of the irradiation event.

U2 - 10.1088/0004-637X/717/2/861

DO - 10.1088/0004-637X/717/2/861

M3 - Journal article

VL - 717

SP - 861

EP - 867

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

ER -

ID: 34202435