¹L. Gavilan, ²C. Jäger, ³A. Simionovici, ⁴J. L. Lemaire, ²T. Sabri, ⁵E. Foy, ⁶S. Yagoubi, ⁷T. Henning, ⁸D. Salomon, ⁸G. Martinez-Criado
Astronomy & Astrophysics 587, A144    Link to Article [http://dx.doi.org/10.1051/0004-6361/201527708]
¹Institut d’Astrophysique Spatiale (IAS), CNRS, Univ. Paris Sud, Université Paris-Saclay, 91405 Orsay, France
e-mail: lisseth.gavilan@ias.u-psud.fr
²Laboratory Astrophysics and Cluster Physics Group of the Max Planck Institute for Astronomy at the Friedrich Schiller University & Institute of Solid State Physics, Helmholtzweg 3, 07743 Jena, Germany
³Institut des Sciences de la Terre, Observatoire des Sciences de l’Univers de Grenoble, BP 53, 38041 Grenoble, France
⁴Institut des Sciences Moléculaires d’Orsay (ISMO), CNRS, Univ. Paris Sud, Université Paris-Saclay, 91405 Orsay, France
⁵LAPA-IRAMAT, NIMBE, CEA, CNRS, Université Paris-Saclay, CEA Saclay, 91191 Gif-sur-Yvette, France
⁶LEEL, NIMBE, CEA, CNRS, Université Paris-Saclay, CEA Saclay, 91191 Gif-sur-Yvette, France
⁷Max-Planck Institute for Astronomy Königstuhl 17, 69117 Heidelberg, Germany
⁸European Synchrotron Radiation Facility, 71 avenue des Martyrs, 38000 Grenoble, France

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¹A. Basu Sarbadhikari,²E. V. S. S. K. Babu,²T. Vijaya Kumar,³H. Chennaoui Aoudjehane
Meteoritics & Planetary Sciences        Link to Article [DOI: 10.1111/maps.12684]
¹Physical Research Laboratory, Ahmedabad, India
²National Geophysical Research Institute (Council of Scientific and Industrial Research), Hyderabad, India
³Hassan II University Casablanca, Faculty of Sciences, GAIA Laboratory, Maârif, Casablanca, Morocco
Published by arrangement with John Wiley & Sons

Tissint, a new unaltered piece of Martian volcanic materials, is the most silica-poor and Mg-Fe-rich igneous rock among the “depleted” olivine-phyric shergottites. Fe-Mg zoning of olivine suggests equilibrium growth (<0.1 °C h−1) in the range of Fo80–56 and olivine overgrowth (Fo55–18) through a process of rapid disequilibrium (~1.0–5.0 °C h−1). The spatially extended (up to 600 μm) flat-top Fe-Mg profiles of olivine indicates that the early-stage cooling rate of Tissint was slower than the other shergottites. The chemically metastable outer rim of olivine (<Fo55) consists of oscillatory phosphorus zoning at the impact-induced melt domains and grew rapidly compared to the early to intermediate-stage crystallization of the Tissint bulk. High-Ca pyroxene to low-Ca pyroxene and high-Ca pyroxene to plagioclase ratios of Tissint are more comparable to the enriched basaltic and enriched olivine-phyric shergottites. Dominance of augite over plagioclase induced augite to control the Ca-buffer in the residual melt suppressing the plagioclase crystallization, which also caused a profound effect on the Al-content in the late-crystallized pyroxenes. Mineral chemical stability, phase-assemblage saturation, and pressure–temperature path of evolution indicates that the parent magma entered the solidus and left the liquidus field at a depth of 40–80 km in the upper mantle. Petrogenesis of Tissint appears to be similar to LAR 06319, an enriched olivine-phyric shergottite, during the early to intermediate stage of crystallization. A severe shock-induced deformation resulted in remelting (10–15 vol%), recrystallization (most Fe-rich phases), and exhumation of Tissint in a time scale of 1–8 yr. Tissint possesses some distinct characteristics, e.g., impact-induced melting and deformation, forming phosphorus-rich recrystallization rims of olivine, and shock-induced melt domains without relative enrichment of LREEs compared to the bulk; and shared characteristics, e.g., modal composition and magmatic evolution with the enriched basaltic shergottites, evidently reflecting unique mantle source in comparison to the clan of the depleted members.