Magnesium isotope systematics in Martian meteorites

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00025798%3A_____%2F17%3A00000088" target="_blank" >RIV/00025798:_____/17:00000088 - isvavai.cz</a>

Výsledek na webu

<a href="http://www.sciencedirect.com/science/journal/0012821X?sdc=1" target="_blank" >http://www.sciencedirect.com/science/journal/0012821X?sdc=1</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.epsl.2017.07.012" target="_blank" >10.1016/j.epsl.2017.07.012</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Magnesium isotope systematics in Martian meteorites

Popis výsledku v původním jazyce

Magnesium isotope compositions are reported for a suite of Martian meteorites that span the range of petrological and geochemical types recognized for Mars, including crustal breccia NWA 7034. The d26Mg values (per mil units relative to DSM-3 reference material) range from −0.32 to −0.11‰; basaltic shergottites and nakhlites lie to the heavier end of the Mg isotope range whereas olivine-phyric, olivine–orthopyroxene-phyric and lherzolitic shergottites, and chassignites have slightly lighter Mg isotope compositions, attesting to modest correlation of Mg isotopes and petrology of the samples. Slightly heavier Mg isotope compositions found for surface-related materials (NWA 7034, black glass fraction of the Tissint shergottite fall; d26Mg > −0.17‰) indicate measurable Mg isotope difference between the Martian mantle and crust but the true extent of Mg isotope fractionation for Martian surface materials remains unconstrained. The range of d26Mg values from −0.19 to −0.11‰ in nakhlites is most likely due to accumulation of clinopyroxene during petrogenesis rather than garnet fractionation in the source or assimilation of surface material modified at low temperatures. The rather restricted range in Mg isotope compositions between spatially and temporally distinct mantle-derived samples provides evidence for inefficient/absent major tectonic cycles on Mars, which would include plate tectonics and large-scale recycling of isotopically fractionated surface materials back into the Martian mantle. The cumulative d26Mg value of Martian samples, which are not influenced by late-stage alteration and/or crust–mantle interactions, is −0.271 +/- 0.040‰ (2SD) and is considered to reflect d26Mg value of the Bulk Silicate Mars. This value is robust taking into account the range of lithologies involved in this estimate. It also attests to planetary-scale Mg isotope homogeneity in the inner Solar System, noted for several other major elements.

Název v anglickém jazyce

Magnesium isotope systematics in Martian meteorites

Popis výsledku anglicky

Magnesium isotope compositions are reported for a suite of Martian meteorites that span the range of petrological and geochemical types recognized for Mars, including crustal breccia NWA 7034. The d26Mg values (per mil units relative to DSM-3 reference material) range from −0.32 to −0.11‰; basaltic shergottites and nakhlites lie to the heavier end of the Mg isotope range whereas olivine-phyric, olivine–orthopyroxene-phyric and lherzolitic shergottites, and chassignites have slightly lighter Mg isotope compositions, attesting to modest correlation of Mg isotopes and petrology of the samples. Slightly heavier Mg isotope compositions found for surface-related materials (NWA 7034, black glass fraction of the Tissint shergottite fall; d26Mg > −0.17‰) indicate measurable Mg isotope difference between the Martian mantle and crust but the true extent of Mg isotope fractionation for Martian surface materials remains unconstrained. The range of d26Mg values from −0.19 to −0.11‰ in nakhlites is most likely due to accumulation of clinopyroxene during petrogenesis rather than garnet fractionation in the source or assimilation of surface material modified at low temperatures. The rather restricted range in Mg isotope compositions between spatially and temporally distinct mantle-derived samples provides evidence for inefficient/absent major tectonic cycles on Mars, which would include plate tectonics and large-scale recycling of isotopically fractionated surface materials back into the Martian mantle. The cumulative d26Mg value of Martian samples, which are not influenced by late-stage alteration and/or crust–mantle interactions, is −0.271 +/- 0.040‰ (2SD) and is considered to reflect d26Mg value of the Bulk Silicate Mars. This value is robust taking into account the range of lithologies involved in this estimate. It also attests to planetary-scale Mg isotope homogeneity in the inner Solar System, noted for several other major elements.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10505 - Geology

Projekt

<a href="/cs/project/GA13-22351S" target="_blank" >GA13-22351S: Využití netradičních a tradičních izotopových systémů k identifikaci zdrojových materiálů a procesů vzniku vltavínů</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2017

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Earth and Planetary Science Letters

ISSN

0012-821X

e-ISSN

—

Svazek periodika

474

Číslo periodika v rámci svazku

September 15

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

8

Strana od-do

419-426

Kód UT WoS článku

000409150600042

EID výsledku v databázi Scopus

2-s2.0-85025835133