Martian magmatism from plume metasomatized mantle

Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted m...

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Published inNature communications Vol. 9; no. 1; pp. 4799 - 8
Main Authors Day, James M. D., Tait, Kimberly T., Udry, Arya, Moynier, Frédéric, Liu, Yang, Neal, Clive R.
Format Journal Article
LanguageEnglish
Published London Nature Publishing Group UK 15.11.2018
Nature Publishing Group
Nature Portfolio
Subjects
140/58
639/33/445/845
704/445/209
704/445/849
Chassignites
Composition
Depletion
Earth Sciences
Humanities and Social Sciences
Isotopes
Lithosphere
Mars
Melting
Melts
Meteors & meteorites
multidisciplinary
Nakhlites
Petrogenesis
Planetary mantles
Plumes
Science
Science (multidisciplinary)
Sciences of the Universe
Shergottites
SNC meteorites
Terrestrial environments
Volcanic activity
Zirconium
DIFFERENTIATION HISTORY
MAUNA-KEA VOLCANO
MARS
ISOTOPIC SYSTEMATICS
MIDOCEAN RIDGE BASALT
DEPLETED MANTLE
SM-ND
HAWAIIAN HOT-SPOT
REJUVENATED VOLCANISM
RB-SR
Online AccessGet full text

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Abstract Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here we report a coherent geochemical dataset for shergottites, nakhlites and chassignites revealing fundamental differences in sources. Shergottites have lower Nb/Y at a given Zr/Y than nakhlites or chassignites, a relationship nearly identical to terrestrial Hawaiian main shield and rejuvenated volcanism. Nakhlite and chassignite compositions are consistent with melting of hydrated and metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep mantle sources. Generation of martian magmas can be explained by temporally distinct melting episodes within and below dynamically supported and variably metasomatized lithosphere, by long-lived, static mantle plumes. A unified model for the formation of martian rock types is required to understand Mars’s formation and evolution. Here the authors show that nakhlite and chassignite meteorites originate from melting of metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep plume sources.
AbstractList Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here we report a coherent geochemical dataset for shergottites, nakhlites and chassignites revealing fundamental differences in sources. Shergottites have lower Nb/Y at a given Zr/Y than nakhlites or chassignites, a relationship nearly identical to terrestrial Hawaiian main shield and rejuvenated volcanism. Nakhlite and chassignite compositions are consistent with melting of hydrated and meta-somatized depleted mantle lithosphere, whereas shergottite melts originate from deep mantle sources. Generation of martian magmas can be explained by temporally distinct melting episodes within and below dynamically supported and variably metasomatized lithosphere, by long-lived, static mantle plumes.
Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here we report a coherent geochemical dataset for shergottites, nakhlites and chassignites revealing fundamental differences in sources. Shergottites have lower Nb/Y at a given Zr/Y than nakhlites or chassignites, a relationship nearly identical to terrestrial Hawaiian main shield and rejuvenated volcanism. Nakhlite and chassignite compositions are consistent with melting of hydrated and metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep mantle sources. Generation of martian magmas can be explained by temporally distinct melting episodes within and below dynamically supported and variably metasomatized lithosphere, by long-lived, static mantle plumes. A unified model for the formation of martian rock types is required to understand Mars’s formation and evolution. Here the authors show that nakhlite and chassignite meteorites originate from melting of metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep plume sources.
Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here we report a coherent geochemical dataset for shergottites, nakhlites and chassignites revealing fundamental differences in sources. Shergottites have lower Nb/Y at a given Zr/Y than nakhlites or chassignites, a relationship nearly identical to terrestrial Hawaiian main shield and rejuvenated volcanism. Nakhlite and chassignite compositions are consistent with melting of hydrated and metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep mantle sources. Generation of martian magmas can be explained by temporally distinct melting episodes within and below dynamically supported and variably metasomatized lithosphere, by long-lived, static mantle plumes.
Abstract Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here we report a coherent geochemical dataset for shergottites, nakhlites and chassignites revealing fundamental differences in sources. Shergottites have lower Nb/Y at a given Zr/Y than nakhlites or chassignites, a relationship nearly identical to terrestrial Hawaiian main shield and rejuvenated volcanism. Nakhlite and chassignite compositions are consistent with melting of hydrated and metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep mantle sources. Generation of martian magmas can be explained by temporally distinct melting episodes within and below dynamically supported and variably metasomatized lithosphere, by long-lived, static mantle plumes.
A unified model for the formation of martian rock types is required to understand Mars’s formation and evolution. Here the authors show that nakhlite and chassignite meteorites originate from melting of metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep plume sources.
ArticleNumber 4799
Author Liu, Yang
Neal, Clive R.
Moynier, Frédéric
Tait, Kimberly T.
Day, James M. D.
Udry, Arya
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  surname: Neal
  fullname: Neal, Clive R.
  organization: Department of Civil and Environmental Engineering and Earth Science, University of Notre Dame
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Keywords DIFFERENTIATION HISTORY
MAUNA-KEA VOLCANO
MARS
ISOTOPIC SYSTEMATICS
MIDOCEAN RIDGE BASALT
DEPLETED MANTLE
SM-ND
HAWAIIAN HOT-SPOT
REJUVENATED VOLCANISM
RB-SR
Language English
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SSID ssj0000391844
Score 2.530309
Snippet Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites,...
Abstract Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma...
Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites,...
A unified model for the formation of martian rock types is required to understand Mars’s formation and evolution. Here the authors show that nakhlite and...
SourceID doaj
pubmedcentral
hal
proquest
crossref
pubmed
springer
SourceType Open Website
Open Access Repository
Aggregation Database
Index Database
Publisher
StartPage 4799
SubjectTerms 140/58
639/33/445/845
704/445/209
704/445/849
Chassignites
Composition
Depletion
Earth Sciences
Humanities and Social Sciences
Isotopes
Lithosphere
Mars
Melting
Melts
Meteors & meteorites
multidisciplinary
Nakhlites
Petrogenesis
Planetary mantles
Plumes
Science
Science (multidisciplinary)
Sciences of the Universe
Shergottites
SNC meteorites
Terrestrial environments
Volcanic activity
Zirconium
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Title Martian magmatism from plume metasomatized mantle
URI https://link.springer.com/article/10.1038/s41467-018-07191-0
https://www.ncbi.nlm.nih.gov/pubmed/30442916
https://www.proquest.com/docview/2133834797
https://search.proquest.com/docview/2135124039
https://insu.hal.science/insu-02612931
https://pubmed.ncbi.nlm.nih.gov/PMC6237973
https://doaj.org/article/12c5c7c3484041ed8a09d23db1371ab0
Volume 9
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