TY  - JOUR
A1  - Grott, Matthias
A1  - Knollenberg, J.
A1  - Hamm, M.
A1  - Ogawa, K.
A1  - Jaumann, R.
A1  - Otto, Katharina Alexandra
A1  - Delbo, M.
A1  - Michel, Patrick
A1  - Biele, J.
A1  - Neumann, Wladimir
A1  - Knapmeyer, Martin
A1  - Kührt, E.
A1  - Senshu, H.
A1  - Okada, T.
A1  - Helbert, Jorn
A1  - Maturilli, A.
A1  - Müller, N.
A1  - Hagermann, A.
A1  - Sakatani, Naoya
A1  - Tanaka, S.
A1  - Arai, T.
A1  - Mottola, Stefano
A1  - Tachibana, Shogo
A1  - Pelivan, Ivanka
A1  - Drube, Line
A1  - Vincent, J-B
A1  - Yano, Hajime
A1  - Pilorget, C.
A1  - Matz, K. D.
A1  - Schmitz, N.
A1  - Koncz, A.
A1  - Schröder, Stefan E.
A1  - Trauthan, F.
A1  - Schlotterer, Markus
A1  - Krause, C.
A1  - Ho, T-M
A1  - Moussi-Soffys, A.
T1  - Low thermal conductivity boulder with high porosity identified on C-type asteroid (162173) Ryugu
JF  - Nature astronomy
N2  - C-type asteroids are among the most pristine objects in the Solar System, but little is known about their interior structure and surface properties. Telescopic thermal infrared observations have so far been interpreted in terms of a regolith-covered surface with low thermal conductivity and particle sizes in the centimetre range. This includes observations of C-type asteroid (162173) Ryugu1,2,3. However, on arrival of the Hayabusa2 spacecraft at Ryugu, a regolith cover of sand- to pebble-sized particles was found to be absent4,5 (R.J. et al., manuscript in preparation). Rather, the surface is largely covered by cobbles and boulders, seemingly incompatible with the remote-sensing infrared observations. Here we report on in situ thermal infrared observations of a boulder on the C-type asteroid Ryugu. We found that the boulder’s thermal inertia was much lower than anticipated based on laboratory measurements of meteorites, and that a surface covered by such low-conductivity boulders would be consistent with remote-sensing observations. Our results furthermore indicate high boulder porosities as well as a low tensile strength in the few hundred kilopascal range. The predicted low tensile strength confirms the suspected observational bias6 in our meteorite collections, as such asteroidal material would be too frail to survive atmospheric entry7
Y1  - 2019
U6  - https://doi.org/10.1038/s41550-019-0832-x
SN  - 2397-3366
VL  - 3
IS  - 11
SP  - 971
EP  - 976
PB  - Nature Publishing Group
CY  - London
ER  - 
TY  - JOUR
A1  - Grott, Matthias
A1  - Knollenberg, J.
A1  - Hamm, M.
A1  - Ogawa, K.
A1  - Jaumann, R.
A1  - Otto, Katharina Alexandra
A1  - Delbo, M.
A1  - Michel, P.
A1  - Biele, J.
A1  - Neumann, W.
A1  - Knapmeyer, M.
A1  - Kuehrt, E.
A1  - Senshu, H.
A1  - Okada, T.
A1  - Helbert, J.
A1  - Maturilli, A.
A1  - Müller, N.
A1  - Hagermann, A.
A1  - Sakatani, N.
A1  - Tanaka, S.
A1  - Arai, T.
A1  - Mottola, S.
A1  - Tachibana, S.
A1  - Pelivan, Ivanka
A1  - Drube, L.
A1  - Vincent, J-B
A1  - Yano, H.
A1  - Pilorget, C.
A1  - Matz, K. D.
A1  - Schmitz, N.
A1  - Koncz, A.
A1  - Schröder, S. E.
A1  - Trauthan, F.
A1  - Schlotterer, M.
A1  - Krause, C.
A1  - Ho, T-M
A1  - Moussi-Soffys, A.
T1  - Low thermal conductivity boulder with high porosity identified on C-type asteroid (162173) Ryugu
JF  - Nature astronomy
N2  - C-type asteroids are among the most pristine objects in the Solar System, but little is known about their interior structure and surface properties. Telescopic thermal infrared observations have so far been interpreted in terms of a regolith-covered surface with low thermal conductivity and particle sizes in the centimetre range. This includes observations of C-type asteroid (162173) Ryugu1,2,3. However, on arrival of the Hayabusa2 spacecraft at Ryugu, a regolith cover of sand- to pebble-sized particles was found to be absent4,5 (R.J. et al., manuscript in preparation). Rather, the surface is largely covered by cobbles and boulders, seemingly incompatible with the remote-sensing infrared observations. Here we report on in situ thermal infrared observations of a boulder on the C-type asteroid Ryugu. We found that the boulder’s thermal inertia was much lower than anticipated based on laboratory measurements of meteorites, and that a surface covered by such low-conductivity boulders would be consistent with remote-sensing observations. Our results furthermore indicate high boulder porosities as well as a low tensile strength in the few hundred kilopascal range. The predicted low tensile strength confirms the suspected observational bias6 in our meteorite collections, as such asteroidal material would be too frail to survive atmospheric entry7.
Y1  - 2020
U6  - https://doi.org/10.1038/s41550-019-0832-x
SN  - 2397-3366
VL  - 3
IS  - 11
SP  - 971
EP  - 976
PB  - Nature Publishing Group
CY  - London
ER  - 
TY  - JOUR
A1  - Spengler, D.
A1  - Obata, M.
A1  - Hirajima, T.
A1  - Ottolini, L.
A1  - Ohfuji, H.
A1  - Tamura, A.
A1  - Arai, S.
T1  - Exsolution of garnet and clinopyroxene from High-Al Pyroxenes in Xugou Peridotite, Eastern China
JF  - Journal of petrology
N2  - Serpentinized massif peridotite in the Xugou, Su-Lu ultrahigh-pressure (UHP) metamorphic belt, eastern China, preserves texturally old (porphyroclastic) ortho- and clinopyroxene with up to two generations of lamellae of garnet, clinopyroxene and Mg-chromite. Their crystallographic orientation with respect to the host pyroxene is consistent with an origin by solid-state exsolution. Comparison of integrated mineral chemistry with simplified and natural chemical datasets suggests that both aluminous precursor pyroxenes were in equilibrium at a minimum pressure of similar to 4 GPa and within a temperature range of about 1300-1500 degrees C. Steep isopleths of Ca in orthopyroxene imply that exsolution occurred during cooling. Al diffusion modelling suggests growth of widely spaced lamellae in orthopyroxene down to about 900 degrees C. Integrated Al contents between wide lamellae record a minimum of 4 GPa pressure during cooling. Compositionally uniform exsolved minerals were formed at 4 center dot 3 +/- 0 center dot 3 GPa and 730 +/- 30 degrees C and reflect a cratonic geotherm with about 33 mW m(-2) surface heat flow. The peridotite matrix mineral assemblage of olivine + orthopyroxene +/- garnet +/- Mg-chromite +/- clinopyroxene +/- phlogopite records strain-induced recrystallization that partially to completely replaced precursor porphyroclasts. The recrystallized minerals lack lamellar exsolution. Recrystallized orthopyroxene, with Al2O3 at 0 center dot 13 wt %, indicates conditions of 5 center dot 5 +/- 0 center dot 3 GPa and 760 +/- 30 degrees C, which are higher-grade metamorphic conditions than those preserved in the chemically equilibrated exsolution microstructures. Both estimates overlap with the range reported for the Early Mesozoic UHP metamorphism in the region (4 center dot 0-6 center dot 7 GPa and 760-970 degrees C). Major element melt models applied to previously published Xugou peridotite data suggest high degrees of melt extraction (30-35 %) in the garnet peridotite stability field (3-4 center dot 5 GPa) until garnet and clinopyroxene exhaustion. Coincidence in pressure and in the order of temperature of equilibration of precursor pyroxenes and peridotite melting implies that peridotite formation occurred at similar to 135 km depth in the subcontinental lithospheric mantle (SCLM) beneath the Archaean North China Craton. Subsequent refertilization, mineral exsolution and chemical re-equilibration during long-term cooling in the SCLM occurred prior to deformation and incorporation of the mantle fragment into the continental crust during UHP metamorphism at a minimum depth of 170 km. Because the Xugou precursor pyroxenes and peridotite formed at depths greater than the regional SCLM (c. 90 km), we infer that the orogenic peridotite massif formed part of the former hanging wall of the Archaean SCLM, which delaminated after the Late Mesozoic.
KW  - Archaean SCLM
KW  - Grt-Pyx exsolution
KW  - orogenic peridotite
KW  - UHP metamorphism
Y1  - 2012
U6  - https://doi.org/10.1093/petrology/egs023
SN  - 0022-3530
VL  - 53
IS  - 7
SP  - 1477
EP  - 1504
PB  - Oxford Univ. Press
CY  - Oxford
ER  -