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    Rights statement: This is the author’s version of a work that was accepted for publication in Earth and Planetary Science Letters. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Earth and Planetary Science Letters, 564, 2021 DOI: 10.1016/j.epsl.2021.116907

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Degassing of volcanic extrusives on Mercury: Potential contributions to transient atmospheres and buried polar deposits

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Degassing of volcanic extrusives on Mercury : Potential contributions to transient atmospheres and buried polar deposits. / Deutsch, A.N.; Head, J.W.; Parman, S.W.; Wilson, L.; Neumann, G.A.; Lowden, F.

In: Earth and Planetary Science Letters, Vol. 564, 116907, 15.06.2021.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Deutsch, AN, Head, JW, Parman, SW, Wilson, L, Neumann, GA & Lowden, F 2021, 'Degassing of volcanic extrusives on Mercury: Potential contributions to transient atmospheres and buried polar deposits', Earth and Planetary Science Letters, vol. 564, 116907. https://doi.org/10.1016/j.epsl.2021.116907

APA

Deutsch, A. N., Head, J. W., Parman, S. W., Wilson, L., Neumann, G. A., & Lowden, F. (2021). Degassing of volcanic extrusives on Mercury: Potential contributions to transient atmospheres and buried polar deposits. Earth and Planetary Science Letters, 564, [116907]. https://doi.org/10.1016/j.epsl.2021.116907

Vancouver

Deutsch AN, Head JW, Parman SW, Wilson L, Neumann GA, Lowden F. Degassing of volcanic extrusives on Mercury: Potential contributions to transient atmospheres and buried polar deposits. Earth and Planetary Science Letters. 2021 Jun 15;564. 116907. https://doi.org/10.1016/j.epsl.2021.116907

Author

Deutsch, A.N. ; Head, J.W. ; Parman, S.W. ; Wilson, L. ; Neumann, G.A. ; Lowden, F. / Degassing of volcanic extrusives on Mercury : Potential contributions to transient atmospheres and buried polar deposits. In: Earth and Planetary Science Letters. 2021 ; Vol. 564.

Bibtex

@article{834d605de65b4e9faa7ff9f8112b007b,
title = "Degassing of volcanic extrusives on Mercury: Potential contributions to transient atmospheres and buried polar deposits",
abstract = "The surface of Mercury is dominated by extensive, widespread lava plains that formed early in its history. The emplacement of these lavas was accompanied by the release of magmatic volatiles, the bulk of which were lost to space via thermal escape and/or photodissociation. Here we consider the fate of these erupted volatiles by quantifying the volumes of erupted volcanic plains and estimating the associated masses of erupted volatiles. The concentrations and speciation of volatiles in Mercury's magmas are not known with certainty at this time, so we model a wide range of cases, based on existing experimental data and speciation models, at 3–7 log fO2 units below conditions determined by the iron-w{\"u}stite buffer. Cases range from relatively low gas content scenarios (total exsolved gas mass of 9×1015 kg) to high gas content scenarios (total exsolved gas = 5 × 1019 kg). We estimate that the average duration of a transient volcanic atmosphere resulting from a single eruption would be between ∼250 and ∼210,000 years, depending on the volume, degassed volatile content, and eruption rate of an individual eruption, as well as the fO2 conditions of the planet's interior. If a dense transient atmosphere was ever surface-bound long enough for the released volatiles to be transported to and cold-trapped at Mercury's polar regions, those trapped volatiles are predicted to be well-mixed with the regolith, and at least 16 m beneath the surface given regolith gardening rates. These volatiles would have a composition and age distinctly different from those of the H2O-ice deposits observed at the poles of Mercury today. {\textcopyright} 2021 Elsevier B.V.",
keywords = "atmospheres, Mercury, Moon, polar deposits, volcanism, Earth atmosphere, Mercury (metal), Photodissociation, Volcanoes, Case based, Condition, Extrusives, Gas content, Magmatic volatiles, Polar deposits, Thermal escape, Volcanics, Volcanism, Deposits",
author = "A.N. Deutsch and J.W. Head and S.W. Parman and L. Wilson and G.A. Neumann and F. Lowden",
note = "This is the author{\textquoteright}s version of a work that was accepted for publication in Earth and Planetary Science Letters. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Earth and Planetary Science Letters, 564, 2021 DOI: 10.1016/j.epsl.2021.116907 ",
year = "2021",
month = jun,
day = "15",
doi = "10.1016/j.epsl.2021.116907",
language = "English",
volume = "564",
journal = "Earth and Planetary Science Letters",
issn = "0012-821X",
publisher = "Elsevier Science B.V.",

}

RIS

TY - JOUR

T1 - Degassing of volcanic extrusives on Mercury

T2 - Potential contributions to transient atmospheres and buried polar deposits

AU - Deutsch, A.N.

AU - Head, J.W.

AU - Parman, S.W.

AU - Wilson, L.

AU - Neumann, G.A.

AU - Lowden, F.

N1 - This is the author’s version of a work that was accepted for publication in Earth and Planetary Science Letters. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Earth and Planetary Science Letters, 564, 2021 DOI: 10.1016/j.epsl.2021.116907

PY - 2021/6/15

Y1 - 2021/6/15

N2 - The surface of Mercury is dominated by extensive, widespread lava plains that formed early in its history. The emplacement of these lavas was accompanied by the release of magmatic volatiles, the bulk of which were lost to space via thermal escape and/or photodissociation. Here we consider the fate of these erupted volatiles by quantifying the volumes of erupted volcanic plains and estimating the associated masses of erupted volatiles. The concentrations and speciation of volatiles in Mercury's magmas are not known with certainty at this time, so we model a wide range of cases, based on existing experimental data and speciation models, at 3–7 log fO2 units below conditions determined by the iron-wüstite buffer. Cases range from relatively low gas content scenarios (total exsolved gas mass of 9×1015 kg) to high gas content scenarios (total exsolved gas = 5 × 1019 kg). We estimate that the average duration of a transient volcanic atmosphere resulting from a single eruption would be between ∼250 and ∼210,000 years, depending on the volume, degassed volatile content, and eruption rate of an individual eruption, as well as the fO2 conditions of the planet's interior. If a dense transient atmosphere was ever surface-bound long enough for the released volatiles to be transported to and cold-trapped at Mercury's polar regions, those trapped volatiles are predicted to be well-mixed with the regolith, and at least 16 m beneath the surface given regolith gardening rates. These volatiles would have a composition and age distinctly different from those of the H2O-ice deposits observed at the poles of Mercury today. © 2021 Elsevier B.V.

AB - The surface of Mercury is dominated by extensive, widespread lava plains that formed early in its history. The emplacement of these lavas was accompanied by the release of magmatic volatiles, the bulk of which were lost to space via thermal escape and/or photodissociation. Here we consider the fate of these erupted volatiles by quantifying the volumes of erupted volcanic plains and estimating the associated masses of erupted volatiles. The concentrations and speciation of volatiles in Mercury's magmas are not known with certainty at this time, so we model a wide range of cases, based on existing experimental data and speciation models, at 3–7 log fO2 units below conditions determined by the iron-wüstite buffer. Cases range from relatively low gas content scenarios (total exsolved gas mass of 9×1015 kg) to high gas content scenarios (total exsolved gas = 5 × 1019 kg). We estimate that the average duration of a transient volcanic atmosphere resulting from a single eruption would be between ∼250 and ∼210,000 years, depending on the volume, degassed volatile content, and eruption rate of an individual eruption, as well as the fO2 conditions of the planet's interior. If a dense transient atmosphere was ever surface-bound long enough for the released volatiles to be transported to and cold-trapped at Mercury's polar regions, those trapped volatiles are predicted to be well-mixed with the regolith, and at least 16 m beneath the surface given regolith gardening rates. These volatiles would have a composition and age distinctly different from those of the H2O-ice deposits observed at the poles of Mercury today. © 2021 Elsevier B.V.

KW - atmospheres

KW - Mercury

KW - Moon

KW - polar deposits

KW - volcanism

KW - Earth atmosphere

KW - Mercury (metal)

KW - Photodissociation

KW - Volcanoes

KW - Case based

KW - Condition

KW - Extrusives

KW - Gas content

KW - Magmatic volatiles

KW - Polar deposits

KW - Thermal escape

KW - Volcanics

KW - Volcanism

KW - Deposits

U2 - 10.1016/j.epsl.2021.116907

DO - 10.1016/j.epsl.2021.116907

M3 - Journal article

VL - 564

JO - Earth and Planetary Science Letters

JF - Earth and Planetary Science Letters

SN - 0012-821X

M1 - 116907

ER -