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1. Cosmic dust fertilization of glacial prebiotic chemistry on early Earth

Author

Walton, Craig R., Rigley, Jessica K., Lipp, Alexander, Law, Robert, Suttle, Martin D., Schonbachler, Maria, Wyatt, Mark, and Shorttle, Oliver

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Geophysics
Abstract

Earth's surface is deficient in available forms of many elements considered limiting for prebiotic chemistry. In contrast, many extraterrestrial rocky objects are rich in these same elements. Limiting prebiotic ingredients may, therefore, have been delivered by exogenous material; however, the mechanisms by which exogeneous material may be reliably and non-destructively supplied to a planetary surface remains unclear. Today, the flux of extraterrestrial matter to Earth is dominated by fine-grained cosmic dust. Although this material is rarely discussed in a prebiotic context due to its delivery over a large surface area, concentrated cosmic dust deposits are known to form on Earth today due to the action of sedimentary processes. Here we combine empirical constraints on dust sedimentation with dynamical simulations of dust formation and planetary accretion to show that localized sedimentary deposits of cosmic dust could have accumulated in arid environments on early Earth, in particular glacial settings that today produce cryoconite sediments. Our results challenge the widely held assumption that cosmic dust is incapable of fertilizing prebiotic chemistry. Cosmic dust deposits may have plausibly formed on early Earth and acted to fertilize prebiotic chemistry., Comment: 5 figures

Published
2024
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2. Carbonate record of temporal change in oxygen fugacity and gaseous species in asteroid Ryugu

Author

Fujiya, Wataru, Kawasaki, Noriyuki, Nagashima, Kazuhide, Sakamoto, Naoya, O'D. Alexander, Conel M., Kita, Noriko T., Kitajima, Kouki, Abe, Yoshinari, Aleon, Jerome, Amari, Sachiko, Amelin, Yuri, Bajo, Ken-ichi, Bizzarro, Martin, Bouvier, Audrey, Carlson, Richard W., Chaussidon, Marc, Choi, Byeon-Gak, Dauphas, Nicolas, Davis, Andrew M., Di Rocco, Tommaso, Fukai, Ryota, Gautam, Ikshu, Haba, Makiko K., Hibiya, Yuki, Hidaka, Hiroshi, Homma, Hisashi, Hoppe, Peter, Huss, Gary R., Ichida, Kiyohiro, Iizuka, Tsuyoshi, Ireland, Trevor R., Ishikawa, Akira, Itoh, Shoichi, Kleine, Thorsten, Komatani, Shintaro, Krot, Alexander N., Liu, Ming-Chang, Masuda, Yuki, McKeegan, Kevin D., Morita, Mayu, Motomura, Kazuko, Moynier, Frederic, Nakai, Izumi, Nguyen, Ann, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Piani, Laurette, Qin, Liping, Russell, Sara S., Schonbachler, Maria, Tafla, Lauren, Tang, Haolan, Terada, Kentaro, Terada, Yasuko, Usui, Tomohiro, Wada, Sohei, Wadhwa, Meenakshi, Walker, Richard J., Yamashita, Katsuyuki, Yin, Qing-Zhu, Yokoyama, Tetsuya, Yoneda, Shigekazu, Young, Edward D., Yui, Hiroharu, Zhang, Ai-Cheng, Nakamura, Tomoki, Naraoka, Hiroshi, Noguchi, Takaaki, Okazaki, Ryuji, Sakamoto, Kanako, Yabuta, Hikaru, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nishimura, Masahiro, Okada, Tatsuaki, Yada, Toru, Yogata, Kasumi, Nakazawa, Satoru, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Watanabe, Sei-ichiro, Yoshikawa, Makoto, Tachibana, Shogo, Yurimoto, Hisayoshi, Fujiya, Wataru, Kawasaki, Noriyuki, Nagashima, Kazuhide, Sakamoto, Naoya, O'D. Alexander, Conel M., Kita, Noriko T., Kitajima, Kouki, Abe, Yoshinari, Aleon, Jerome, Amari, Sachiko, Amelin, Yuri, Bajo, Ken-ichi, Bizzarro, Martin, Bouvier, Audrey, Carlson, Richard W., Chaussidon, Marc, Choi, Byeon-Gak, Dauphas, Nicolas, Davis, Andrew M., Di Rocco, Tommaso, Fukai, Ryota, Gautam, Ikshu, Haba, Makiko K., Hibiya, Yuki, Hidaka, Hiroshi, Homma, Hisashi, Hoppe, Peter, Huss, Gary R., Ichida, Kiyohiro, Iizuka, Tsuyoshi, Ireland, Trevor R., Ishikawa, Akira, Itoh, Shoichi, Kleine, Thorsten, Komatani, Shintaro, Krot, Alexander N., Liu, Ming-Chang, Masuda, Yuki, McKeegan, Kevin D., Morita, Mayu, Motomura, Kazuko, Moynier, Frederic, Nakai, Izumi, Nguyen, Ann, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Piani, Laurette, Qin, Liping, Russell, Sara S., Schonbachler, Maria, Tafla, Lauren, Tang, Haolan, Terada, Kentaro, Terada, Yasuko, Usui, Tomohiro, Wada, Sohei, Wadhwa, Meenakshi, Walker, Richard J., Yamashita, Katsuyuki, Yin, Qing-Zhu, Yokoyama, Tetsuya, Yoneda, Shigekazu, Young, Edward D., Yui, Hiroharu, Zhang, Ai-Cheng, Nakamura, Tomoki, Naraoka, Hiroshi, Noguchi, Takaaki, Okazaki, Ryuji, Sakamoto, Kanako, Yabuta, Hikaru, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nishimura, Masahiro, Okada, Tatsuaki, Yada, Toru, Yogata, Kasumi, Nakazawa, Satoru, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Watanabe, Sei-ichiro, Yoshikawa, Makoto, Tachibana, Shogo, and Yurimoto, Hisayoshi

Abstract

The Hayabusa2 spacecraft explored asteroid Ryugu and brought its surface materials to Earth. Ryugu samples resemble Ivuna-type (CI) chondrites-the most chemically primitive meteorites-and contain secondary phyllosilicates and carbonates, which are indicative of aqueous alteration. Understanding the conditions (such as temperature, redox state and fluid composition) during aqueous alteration is crucial to elucidating how Ryugu evolved to its present state, but little is known about the temporal changes in these conditions. Here we show that calcium carbonate (calcite) grains in Ryugu and Ivuna samples have variable O-18/O-16 and C-13/C-12 ratios that are, respectively, 24-46 & PTSTHOUSND; and 65-108 & PTSTHOUSND; greater than terrestrial standard values, whereas those of calcium-magnesium carbonate (dolomite) grains are much more homogeneous, ranging within 31-36 & PTSTHOUSND; for oxygen and 67-75 & PTSTHOUSND; for carbon. We infer that the calcite precipitated first over a wide range of temperatures and oxygen partial pressures, and that the proportion of gaseous CO2/CO/CH4 molecules changed temporally. By contrast, the dolomite formed later in a more oxygen-rich and thus CO2-dominated environment when the system was approaching equilibrium. The characteristic isotopic compositions of secondary carbonates in Ryugu and Ivuna are not observed for other hydrous meteorites, suggesting a unique evolutionary pathway for their parent asteroid(s). The asteroid Ryugu experienced aqueous alteration under changing temperature and redox conditions, according to an isotopic analysis of secondary calcite and dolomite grains in samples from Ryugu obtained by the Hayabusa2 spacecraft.

Published
2023

3. The Sariçiçek Howardite Fall in Turkey: Source Crater of HED Meteorites on Vesta and Impact Risk of Vestoids

Author

Unsalan, Ozan, Jenniskens, Peter, Yin, Qing-Zhu, Kaygisiz, Ersin, Albers, Jim, Clark, David L, Granvik, Mikael, Demirkol, Iskender, Erdogan, Ibrahim Y, Bengu, Aydin S, Ozel, Mehmet E, Terzioglu, Zahide, Gi, Nayeob, Brown, Peter, Yalcinkaya, Esref, Temel, Tu_Gba, Prabhu, Dinesh K, Robertson, Darrel K, Boslough, Mark, Ostrowski, Daniel R, Kimberley, Jamie, Er, Selman, Rowland, Douglas J, Bryson, Kathryn L, Altunayar-Unsalan, Cisem, Ranguelov, Bogdan, Karamanov, Alexander, Tatchev, Dragomir, Kocahan, Ozlem, Oshtrakh, Michael I, Maksimova, Alevtina A, Karabanalov, Maxim S, Verosub, Kenneth L, Levin, Emily, Uysal, Ibrahim, Hoffmann, Viktor, Hiroi, Takahiro, Reddy, Vishnu, Ildiz, Gulce O, Bolukbasi, Olcay, Zolensky, Michael E, Hochleitner, Rupert, Kaliwoda, Melanie, Ongen, Sinan, Fausto, Rui, Nogueira, Bernardo A, Chukin, Andrey V, Karashanova, Daniela, Semionkin, Vladimir A, Yes_Iltas_, Mehmet, Glotch, Timothy, Yilmaz, Ayberk, Friedrich, Jon M, Sanborn, Matthew E, Huyskens, Magdalena, Ziegler, Karen, Williams, Curtis D, Schonbachler, Maria, Bauer, Kerstin, Meier, Matthias M. M, Maden, Colin, Busemann, Henner, Welten, Kees C, Caffee, Marc W, Laubenstein, Matthias, Zhou, Qin, Li, Qiu-Li, Li, Xian-Hua, Liu, Yu, Tang, Guo- Qiang, Sears, Derek W. G, Mclain, Hannah L, Dworkin, Jason P, Elsila, Jamie E, Glavin, Daniel P, Schmitt-Kopplin, Philippe, Ruf, Alexander, Corre, Lucille Le, and Schmedemann, Nico

Subjects
Space Sciences (General)
Abstract

The Sariçiçek howardite meteorite shower consisting of 343 documented stones occurred on September 2, 2015 in Turkey and is the first documented howardite fall. Cosmogenic isotopes show that Sariçiçek experienced a complex cosmic‐ray exposure history, exposed during ~12–14 Ma in a regolith near the surface of a parent asteroid, and that an ~1 m sized meteoroid was launched by an impact 22 ± 2 Ma ago to Earth (as did one‐third of all HED meteorites). SIMS dating of zircon and baddeleyite yielded 4550.4 ± 2.5 Ma and 4553 ± 8.8 Ma crystallization ages for the basaltic magma clasts. The apatite U‐Pb age of 4525 ± 17 Ma, K‐Ar age of ~3.9 Ga, and the U,Th‐He ages of 1.8 ± 0.7 and 2.6 ± 0.3 Ga are interpreted to represent thermal metamorphic and impact‐related resetting ages, respectively. Petrographic; geochemical; and O‐, Cr‐, and Ti‐isotopic studies confirm that Sariçiçek belongs to the normal clan of HED meteorites. Petrographic observations and analysis of organic material indicate a small portion of carbonaceous chondrite material in the Sariçiçek regolith and organic contamination of the meteorite after a few days on soil. Video observations of the fall show an atmospheric entry at 17.3 ± 0.8 km/s from NW; fragmentations at 37, 33, 31, and 27 km altitude; and provide a pre‐atmospheric orbit that is the first dynamical link between the normal HED meteorite clan and the inner Main Belt. Spectral data indicate the similarity of Sariçiçek with the Vesta asteroid family (V‐class) spectra, a group of asteroids stretching to delivery resonances, which includes (4) Vesta. Dynamical modeling of meteoroid delivery to Earth shows that the complete disruption of a ~1 km sized Vesta family asteroid or a ~10 km sized impact crater on Vesta is required to provide sufficient meteoroids ≤4 m in size to account for the influx of meteorites from this HED clan. The 16.7 km diameter Antionia impact crater on Vesta was formed on terrain of the same age as given by the 4He retention age of Sariçiçek. Lunar scaling for crater production to crater counts of its ejecta blanketshow it was formed ~22 Ma ago.

Published
2019
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4. Oxygen isotopes of anhydrous primary minerals show kinship between asteroid Ryugu and comet 81P/Wild2

Author

1000050770278, Kawasaki, Noriyuki, Nagashima, Kazuhide, Sakamoto, Naoya, Matsumoto, Toru, Bajo, Ken-Ichi, Wada, Sohei, Igami, Yohei, Miyake, Akira, Noguchi, Takaaki, Yamamoto, Daiki, Russell, Sara S., Abe, Yoshinari, Aleon, Jerome, Alexander, Conel M. O'd, Amari, Sachiko, Amelin, Yuri, Bizzarro, Martin, Bouvier, Audrey, Carlson, Richard W., Chaussidon, Marc, Choi, Byeon-Gak, Dauphas, Nicolas, Davis, Andrew M., Di Rocco, Tommaso, Fujiya, Wataru, Fukai, Ryota, Gautam, Ikshu, Haba, Makiko K., Hibiya, Yuki, Hidaka, Hiroshi, Homma, Hisashi, Hoppe, Peter, Huss, Gary R., Ichida, Kiyohiro, Iizuka, Tsuyoshi, Ireland, Trevor R., Ishikawa, Akira, Ito, Motoo, Itoh, Shoichi, Kita, Noriko T., Kitajima, Kouki, Kleine, Thorsten, Komatani, Shintaro, Krot, Alexander N., Liu, Ming-Chang, Masuda, Yuki, McKeegan, Kevin D., Morita, Mayu, Motomura, Kazuko, Moynier, Frederic, Nakai, Izumi, Nguyen, Ann, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Piani, Laurette, Qin, Liping, Schonbachler, Maria, Tafla, Lauren, Tang, Haolan, Terada, Kentaro, Terada, Yasuko, Usui, Tomohiro, Wadhwa, Meenakshi, Walker, Richard J., Yamashita, Katsuyuki, Yin, Qing-Zhu, Yokoyama, Tetsuya, Yoneda, Shigekazu, Young, Edward D., Yui, Hiroharu, Zhang, Ai-Cheng, Nakamura, Tomoki, Naraoka, Hiroshi, Okazaki, Ryuji, Sakamoto, Kanako, Yabuta, Hikaru, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nishimura, Masahiro, Okada, Tatsuaki, Yada, Toru, Yogata, Kasumi, Nakazawa, Satoru, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Watanabe, Sei-Ichiro, Yoshikawa, Makoto, Tachibana, Shogo, Yurimoto, Hisayoshi, 1000050770278, Kawasaki, Noriyuki, Nagashima, Kazuhide, Sakamoto, Naoya, Matsumoto, Toru, Bajo, Ken-Ichi, Wada, Sohei, Igami, Yohei, Miyake, Akira, Noguchi, Takaaki, Yamamoto, Daiki, Russell, Sara S., Abe, Yoshinari, Aleon, Jerome, Alexander, Conel M. O'd, Amari, Sachiko, Amelin, Yuri, Bizzarro, Martin, Bouvier, Audrey, Carlson, Richard W., Chaussidon, Marc, Choi, Byeon-Gak, Dauphas, Nicolas, Davis, Andrew M., Di Rocco, Tommaso, Fujiya, Wataru, Fukai, Ryota, Gautam, Ikshu, Haba, Makiko K., Hibiya, Yuki, Hidaka, Hiroshi, Homma, Hisashi, Hoppe, Peter, Huss, Gary R., Ichida, Kiyohiro, Iizuka, Tsuyoshi, Ireland, Trevor R., Ishikawa, Akira, Ito, Motoo, Itoh, Shoichi, Kita, Noriko T., Kitajima, Kouki, Kleine, Thorsten, Komatani, Shintaro, Krot, Alexander N., Liu, Ming-Chang, Masuda, Yuki, McKeegan, Kevin D., Morita, Mayu, Motomura, Kazuko, Moynier, Frederic, Nakai, Izumi, Nguyen, Ann, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Piani, Laurette, Qin, Liping, Schonbachler, Maria, Tafla, Lauren, Tang, Haolan, Terada, Kentaro, Terada, Yasuko, Usui, Tomohiro, Wadhwa, Meenakshi, Walker, Richard J., Yamashita, Katsuyuki, Yin, Qing-Zhu, Yokoyama, Tetsuya, Yoneda, Shigekazu, Young, Edward D., Yui, Hiroharu, Zhang, Ai-Cheng, Nakamura, Tomoki, Naraoka, Hiroshi, Okazaki, Ryuji, Sakamoto, Kanako, Yabuta, Hikaru, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nishimura, Masahiro, Okada, Tatsuaki, Yada, Toru, Yogata, Kasumi, Nakazawa, Satoru, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Watanabe, Sei-Ichiro, Yoshikawa, Makoto, Tachibana, Shogo, and Yurimoto, Hisayoshi

Abstract

The extraterrestrial materials returned from asteroid (162173) Ryugu consist predominantly of low-temperature aqueously formed secondary minerals and are chemically and mineralogically similar to CI (Ivuna-type) carbonaceous chondrites. Here, we show that high-temperature anhydrous primary minerals in Ryugu and CI chondrites exhibit a bimodal distribution of oxygen isotopic compositions: 16O-rich (associated with refractory inclusions) and 16O-poor (associated with chondrules). Both the 16O-rich and 16O-poor minerals probably formed in the inner solar protoplanetary disk and were subsequently transported outward. The abundance ratios of the 16O-rich to 16O-poor minerals in Ryugu and CI chondrites are higher than in other carbonaceous chondrite groups but are similar to that of comet 81P/Wild2, suggesting that Ryugu and CI chondrites accreted in the outer Solar System closer to the accretion region of comets.

Published
2022

5. Oxygen isotopes of anhydrous primary minerals show kinship between asteroid Ryugu and comet 81P/Wild2

Author

Kawasaki, Noriyuki, Nagashima, Kazuhide, Sakamoto, Naoya, Matsumoto, Toru, Bajo, Ken-Ichi, Wada, Sohei, Igami, Yohei, Miyake, Akira, Noguchi, Takaaki, Yamamoto, Daiki, Russell, Sara S., Abe, Yoshinari, Aleon, Jerome, Alexander, Conel M. O'd, Amari, Sachiko, Amelin, Yuri, Bizzarro, Martin, Bouvier, Audrey, Carlson, Richard W., Chaussidon, Marc, Choi, Byeon-Gak, Dauphas, Nicolas, Davis, Andrew M., Di Rocco, Tommaso, Fujiya, Wataru, Fukai, Ryota, Gautam, Ikshu, Haba, Makiko K., Hibiya, Yuki, Hidaka, Hiroshi, Homma, Hisashi, Hoppe, Peter, Huss, Gary R., Ichida, Kiyohiro, Iizuka, Tsuyoshi, Ireland, Trevor R., Ishikawa, Akira, Ito, Motoo, Itoh, Shoichi, Kita, Noriko T., Kitajima, Kouki, Kleine, Thorsten, Komatani, Shintaro, Krot, Alexander N., Liu, Ming-Chang, Masuda, Yuki, McKeegan, Kevin D., Morita, Mayu, Motomura, Kazuko, Moynier, Frederic, Nakai, Izumi, Nguyen, Ann, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Piani, Laurette, Qin, Liping, Schonbachler, Maria, Tafla, Lauren, Tang, Haolan, Terada, Kentaro, Terada, Yasuko, Usui, Tomohiro, Wadhwa, Meenakshi, Walker, Richard J., Yamashita, Katsuyuki, Yin, Qing-Zhu, Yokoyama, Tetsuya, Yoneda, Shigekazu, Young, Edward D., Yui, Hiroharu, Zhang, Ai-Cheng, Nakamura, Tomoki, Naraoka, Hiroshi, Okazaki, Ryuji, Sakamoto, Kanako, Yabuta, Hikaru, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nishimura, Masahiro, Okada, Tatsuaki, Yada, Toru, Yogata, Kasumi, Nakazawa, Satoru, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Watanabe, Sei-Ichiro, Yoshikawa, Makoto, Tachibana, Shogo, Yurimoto, Hisayoshi, Kawasaki, Noriyuki, Nagashima, Kazuhide, Sakamoto, Naoya, Matsumoto, Toru, Bajo, Ken-Ichi, Wada, Sohei, Igami, Yohei, Miyake, Akira, Noguchi, Takaaki, Yamamoto, Daiki, Russell, Sara S., Abe, Yoshinari, Aleon, Jerome, Alexander, Conel M. O'd, Amari, Sachiko, Amelin, Yuri, Bizzarro, Martin, Bouvier, Audrey, Carlson, Richard W., Chaussidon, Marc, Choi, Byeon-Gak, Dauphas, Nicolas, Davis, Andrew M., Di Rocco, Tommaso, Fujiya, Wataru, Fukai, Ryota, Gautam, Ikshu, Haba, Makiko K., Hibiya, Yuki, Hidaka, Hiroshi, Homma, Hisashi, Hoppe, Peter, Huss, Gary R., Ichida, Kiyohiro, Iizuka, Tsuyoshi, Ireland, Trevor R., Ishikawa, Akira, Ito, Motoo, Itoh, Shoichi, Kita, Noriko T., Kitajima, Kouki, Kleine, Thorsten, Komatani, Shintaro, Krot, Alexander N., Liu, Ming-Chang, Masuda, Yuki, McKeegan, Kevin D., Morita, Mayu, Motomura, Kazuko, Moynier, Frederic, Nakai, Izumi, Nguyen, Ann, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Piani, Laurette, Qin, Liping, Schonbachler, Maria, Tafla, Lauren, Tang, Haolan, Terada, Kentaro, Terada, Yasuko, Usui, Tomohiro, Wadhwa, Meenakshi, Walker, Richard J., Yamashita, Katsuyuki, Yin, Qing-Zhu, Yokoyama, Tetsuya, Yoneda, Shigekazu, Young, Edward D., Yui, Hiroharu, Zhang, Ai-Cheng, Nakamura, Tomoki, Naraoka, Hiroshi, Okazaki, Ryuji, Sakamoto, Kanako, Yabuta, Hikaru, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nishimura, Masahiro, Okada, Tatsuaki, Yada, Toru, Yogata, Kasumi, Nakazawa, Satoru, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Watanabe, Sei-Ichiro, Yoshikawa, Makoto, Tachibana, Shogo, and Yurimoto, Hisayoshi

Abstract

The extraterrestrial materials returned from asteroid (162173) Ryugu consist predominantly of low-temperature aqueously formed secondary minerals and are chemically and mineralogically similar to CI (Ivuna-type) carbonaceous chondrites. Here, we show that high-temperature anhydrous primary minerals in Ryugu and CI chondrites exhibit a bimodal distribution of oxygen isotopic compositions: 16O-rich (associated with refractory inclusions) and 16O-poor (associated with chondrules). Both the 16O-rich and 16O-poor minerals probably formed in the inner solar protoplanetary disk and were subsequently transported outward. The abundance ratios of the 16O-rich to 16O-poor minerals in Ryugu and CI chondrites are higher than in other carbonaceous chondrite groups but are similar to that of comet 81P/Wild2, suggesting that Ryugu and CI chondrites accreted in the outer Solar System closer to the accretion region of comets.

Published
2022

6. The old, unique C1 chondrite Flensburg - Insight into the first processes of aqueous alteration, brecciation, and the diversity of water-bearing parent bodies and lithologies

Author

Bischoff, Addi, Alexander, Conel M. O'D, Barrat, Jean-alix, Burkhardt, Christoph, Busemann, Henner, Degering, Detlev, Di Rocco, Tommaso, Fischer, Meike, Fockenberg, Thomas, Foustoukos, Dionysis, I, Gattacceca, Jerome, Godinho, Jose R. A., Harries, Dennis, Heinlein, Dieter, Hellmann, Jan L., Hertkorn, Norbert, Holm, Anja, Jull, A. J. Timothy, Kerraouch, Imene, King, Ashley J., Kleine, Thorsten, Koll, Dominik, Lachner, Johannes, Ludwig, Thomas, Merchel, Silke, Mertens, Cornelia A. K., Morino, Precillia, Neumann, Wladimir, Pack, Andreas, Patzek, Markus, Pavetich, Stefan, Reitze, Maximilian P., Rufenacht, Miriam, Rugel, Georg, Schmidt, Charlotte, Schmitt-kopplin, Philippe, Schonbachler, Maria, Trieloff, Mario, Wallner, Anton, Wimmer, Karl, Woelfer, Elias, Bischoff, Addi, Alexander, Conel M. O'D, Barrat, Jean-alix, Burkhardt, Christoph, Busemann, Henner, Degering, Detlev, Di Rocco, Tommaso, Fischer, Meike, Fockenberg, Thomas, Foustoukos, Dionysis, I, Gattacceca, Jerome, Godinho, Jose R. A., Harries, Dennis, Heinlein, Dieter, Hellmann, Jan L., Hertkorn, Norbert, Holm, Anja, Jull, A. J. Timothy, Kerraouch, Imene, King, Ashley J., Kleine, Thorsten, Koll, Dominik, Lachner, Johannes, Ludwig, Thomas, Merchel, Silke, Mertens, Cornelia A. K., Morino, Precillia, Neumann, Wladimir, Pack, Andreas, Patzek, Markus, Pavetich, Stefan, Reitze, Maximilian P., Rufenacht, Miriam, Rugel, Georg, Schmidt, Charlotte, Schmitt-kopplin, Philippe, Schonbachler, Maria, Trieloff, Mario, Wallner, Anton, Wimmer, Karl, and Woelfer, Elias

Abstract

On September 12, 2019 at 12:49:48 (UT) a bolide was observed by hundreds of eye-witnesses from the Netherlands, Germany, Belgium, Denmark and the UK. One day later a small meteorite stone was found by accident in Flensburg. The presence of short-lived cosmogenic radionuclides with half-lives as short as 16 days proves the recent exposure of the found object to cosmic rays in space linking it clearly to the bolide event. An exceptionally short exposure time of similar to 5000 years was determined. The 24.5 g stone has a fresh black fusion crust, a low density of <2 g/cm(3), and a magnetic susceptibility of log chi = 4.35 (chi in 10(-9) m(3)/kg). The rock consists of relict chondrules and clusters of sulfide and magnetite grains set in a fine-grained matrix. The most abundant phases are phyllosilicates. Carbonates (similar to 3.9 vol.%) occur as calcites, dolomites, and a Na-rich phase. The relict chondrules (often surrounded by sulfide laths) are free of anhydrous silicates and contain abundant serpentine. Lithic clasts are also surrounded by similar sulfide laths partly intergrown with carbonates. Mn-53-Cr-53 ages of carbonates in Flensburg indicate that brecciation and contemporaneous formation of the pyrrhotite-carbonate intergrowths by hydrothermal activities occurred no later than 4564.6 +/- 1.0 Ma (using the angrite D'Orbigny as the Mn-Cr age anchor). This corresponds to 2.6 +/- 1.0 or 3.4 +/- 1.0 Ma after formation of CAIs, depending on the exact absolute age of CAIs. This is the oldest dated evidence for brecciation and carbonate formation, which likely occurred during parent body growth and incipient heating due to decay of Al-26. In the three oxygen isotope diagram, Flensburg plots at the O-16-rich end of the CM chondrite field and in the transition field to CV-CK-CR chondrites. The mass-dependent Te isotopic composition of Flensburg is slightly different from mean CM chondrites and is most similar to those of the ungrouped C2 chondrite Tagish Lake. On the

Published
2021
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9. Niobium-zirconium chronometry and early solar system development. (Reports)

Author

Schonbachler, Maria, Rehkamper, Mark, Halliday, Alex N., Lee, Der-Chuen, Bourot-Denise, Michele, Zanda, Brigitte, Hattendorf, Bodo, and Gunther, Detlef

Subjects
Nucleosynthesis -- Analysis -- Research, Cosmochemistry -- Research -- Analysis, Solar system -- Research -- Analysis, Science and technology, Analysis, Research
Abstract

Niobium-92 ([sup.92]Nb) decays to zirconium-92 ([sup.92]Zr) with a half-life of 36 million years and can be used to place constraints on the site of p-process nucleosynthesis and the timing of early solar system processes. Recent results have suggested that the initial [sup.92]Nb/[sup.93]Nb of the solar system was high (> [10.sup.-3]). We report Nb-Zr internal isochrons for the ordinary chondrite Estacado (H6) and a clast of the mesosiderite Vaca Muerta, both of which define an initial [sup.92]Nb/ [sup.93]Nb ratio of ~[10.sup.-5]. Therefore, the solar system appears to have started with a ratio of, Some extinct radionuclides were sufficiently abundant at the start of the solar system that they produced variations in the abundance of their daughter isotopes in early-formed objects (1). Such nuclides [...]

Published
2002

10. Simultaneous ultratrace determination of Zr and Nb in chromium matrixes with ICP-dynamic reaction cell MS

Author

Hattendorf, Bodo, Gunther, Detlef, Schonbachler, Maria, and Halliday, Alex

Subjects
Chemistry, Analytic -- Research, Chromium -- Research, Mass spectrometry -- Usage, Zirconium -- Measurement, Niobium -- Measurement, Metallic composites -- Analysis, Chemistry
Abstract

A dynamic reaction cell (DRC) has been used to minimize the formation of metal-argide ions in inductively coupled plasma mass spectrometry and applied to the determination of Zr and Nb in Cr-rich samples. The formation of Ar[Cr.sup.+] species from the plasma gas and the sample matrix was reduced by ion molecule reactions inside a DRC of the ICPMS used. Hydrogen was used as reaction gas, and the efficiency in the reduction of Ar[Cr.sup.+] was similar to that of other plasma-based polyatomic ions as reported in an earlier study. The formation of Cr[O.sub.x.sup.+] ions is enhanced when the DRC is operated in pressurized mode. Adjustment of the transmission properties of the band-pass quadrupole to reject precursor ions can be achieved without dramatic decrease of sensitivity but with a significant improvement in the signal/background ratio. Measurements in solutions containing concentrations of up to 2 g/L Cr showed that the determination of Nb and Zr is possible in the nanogram per liter range in such a matrix. The limits of detection for Nb and Zr in pure Cr metal have been estimated at 2 ng/g for Nb and 5 ng/g for Zr. Analysis of basaltic reference samples resulted in very good agreement with previously published data.

Published
2001

11. The Renchen L5-6 chondrite breccia - The first confirmed meteorite fall from Baden-Wurttemberg (Germany)

Author

Bischoff, Addi, Barrat, Jean-alix, Berndt, Jasper, Borovicka, Jiri, Burkhardt, Christoph, Busemann, Henner, Hakenmueller, Janina, Heinlein, Dieter, Hertzog, Jasmine, Kaiser, Jozef, Maden, Colin, Meier, Matthias M. M., Morino, Precillia, Pack, Andreas, Patzek, Markus, Reitze, Maximilian P., Rufenacht, Miriam, Schmitt-kopplin, Philippe, Schonbachler, Maria, Spurny, Pavel, Weber, Iris, Wimmer, Karl, Zikmund, Tomas, Bischoff, Addi, Barrat, Jean-alix, Berndt, Jasper, Borovicka, Jiri, Burkhardt, Christoph, Busemann, Henner, Hakenmueller, Janina, Heinlein, Dieter, Hertzog, Jasmine, Kaiser, Jozef, Maden, Colin, Meier, Matthias M. M., Morino, Precillia, Pack, Andreas, Patzek, Markus, Reitze, Maximilian P., Rufenacht, Miriam, Schmitt-kopplin, Philippe, Schonbachler, Maria, Spurny, Pavel, Weber, Iris, Wimmer, Karl, and Zikmund, Tomas

Abstract

On July 10, 2018 at 21:29 UT extended areas of South-Western Germany were illuminated by a very bright bolide. This fireball was recorded by instruments of the European Fireball Network (EN). The records enabled complex and precise description of this event including the prediction of the impact area. So far six meteorites totaling about 1.23 kg have been found in the predicted location for a given mass during dedicated searches. The first piece of about 12 g was recovered on July 24 close to the village of Renchen (Baden-Wurttemberg) followed by the largest fragment of 955 g on July 31 about five km north-west of Renchen. Renchen is a moderately-shocked (S4) breccia consisting of abundant highly recrystallized rock fragments as well as impact melt rock clasts. The texture, the large grain size of plagioclase, and the homogeneous compositions of olivine (similar to Fa(26)) and pyroxene (similar to Fs(22)) clearly indicate that Renchen is composed of metamorphosed rock fragments (L5-6). An L-group (and ordinary chondrite) heritage is consistent with the data on the model abundance of metal, the density, the magnetic susceptibility as well as on O-, Ti-, and Cr-isotope characteristics. Renchen does not contain solar wind implanted noble gases and is a fragmental breccia. An unusually large mm-sized merrillite-apatite aggregate shows trace element characteristics like other phosphates from ordinary chondrites. Data on the bulk chemistry, IR-spectroscopy, cosmogenic nuclides, and organic components also indicate similarities to other metamorphosed L chondrites. Noble gas studies reveal that the meteorite has a cosmic ray exposure (CRE) age of 42 Ma and that most of the cosmogenic gases were produced in a meteoroid with a radius of at max. 20 cm based on the radionuclide Al-26 and 10-150 cm based on cosmogenic Ne-22/Ne-21. K-Ar and U/Th-He gas retention ages are both in the range similar to 3.0-3.2 Ga. Both systems do not show evidence for a complete reset 470 Ma ago, an

Published
2019
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12. Evidence for extremely rapid magma ocean crystallization and crust formation on Mars

Author

Bouvier, Laura, Costa, Maria, Connelly, James, Jensen, Ninna, Wielandt, Daniel, Storey, Michael, Nemchin, Alexander, Whitehouse, Martin, Snape, Joshua, Bellucci, Jeremy, Moynier, Frederic, Agranier, Arnaud, Gueguen, Bleuenn, Schonbachler, Maria, Bizzarro, Martin, Bouvier, Laura, Costa, Maria, Connelly, James, Jensen, Ninna, Wielandt, Daniel, Storey, Michael, Nemchin, Alexander, Whitehouse, Martin, Snape, Joshua, Bellucci, Jeremy, Moynier, Frederic, Agranier, Arnaud, Gueguen, Bleuenn, Schonbachler, Maria, and Bizzarro, Martin

Abstract

The formation of a primordial crust is a critical step in the evolution of terrestrial planets but the timing of this process is poorly understood. The mineral zircon is a powerful tool for constraining crust formation because it can be accurately dated with the uranium-to-lead (U–Pb) isotopic decay system and is resistant to subsequent alteration. Moreover, given the high concentration of hafnium in zircon, the lutetium-to-hafnium (176Lu–176Hf) isotopic decay system can be used to determine the nature and formation timescale of its source reservoir (1,2,3) Ancient igneous zircons with crystallization ages of around 4,430 million years (Myr) have been reported in Martian meteorites that are believed to represent regolith breccias from the southern highlands of Mars (4,5) These zircons are present in evolved lithologies interpreted to reflect re-melted primary Martian crust4, thereby potentially providing insight into early crustal evolution on Mars. Here, we report concomitant high-precision U–Pb ages and Hf-isotope compositions of ancient zircons from the NWA 7034 Martian regolith breccia. Seven zircons with mostly concordant U–Pb ages define 207Pb/206Pb dates ranging from 4,476.3 ± 0.9 Myr ago to 4,429.7 ± 1.0 Myr ago, including the oldest directly dated material from Mars. All zircons record unradiogenic initial Hf-isotope compositions inherited from an enriched, andesitic-like crust extracted from a primitive mantle no later than 4,547 Myr ago. Thus, a primordial crust existed on Mars by this time and survived for around 100 Myr before it was reworked, possibly by impacts (4,5) to produce magmas from which the zircons crystallized. Given that formation of a stable primordial crust is the end product of planetary differentiation, our data require that the accretion, core formation and magma ocean crystallization on Mars were completed less than 20 Myr after the formation of the Solar System. These timescales support models that suggest extremely rapid magma ocean

Published
2018
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13. The Stubenberg meteorite-An LL6 chondrite fragmental breccia recovered soon after precise prediction of the strewn field

Author

Bischoff, Addi, Barrat, Jean-alix, Bauer, Kerstin, Burkhardt, Christoph, Busemann, Henner, Ebert, Samuel, Gonsior, Michael, Hakenmueller, Janina, Haloda, Jakub, Harries, Dennis, Heinlein, Dieter, Hiesinger, Harald, Hochleitner, Rupert, Hoffmann, Viktor, Kaliwoda, Melanie, Laubenstein, Matthias, Maden, Colin, Meier, Matthias M. M., Morlok, Andreas, Pack, Andreas, Ruf, Alexander, Schmitt-kopplin, Philippe, Schonbachler, Maria, Steele, Robert C. J., Spurny, Pavel, Wimmer, Karl, Bischoff, Addi, Barrat, Jean-alix, Bauer, Kerstin, Burkhardt, Christoph, Busemann, Henner, Ebert, Samuel, Gonsior, Michael, Hakenmueller, Janina, Haloda, Jakub, Harries, Dennis, Heinlein, Dieter, Hiesinger, Harald, Hochleitner, Rupert, Hoffmann, Viktor, Kaliwoda, Melanie, Laubenstein, Matthias, Maden, Colin, Meier, Matthias M. M., Morlok, Andreas, Pack, Andreas, Ruf, Alexander, Schmitt-kopplin, Philippe, Schonbachler, Maria, Steele, Robert C. J., Spurny, Pavel, and Wimmer, Karl

Abstract

On March 6, 2016 at 21: 36: 51 UT, extended areas of Upper Austria, Bavaria (Germany) and the southwestern part of the Czech Republic were illuminated by a very bright bolide. This bolide was recorded by instruments in the Czech part of the European Fireball Network and it enabled complex and precise description of this event including prediction of the impact area. So far six meteorites totaling 1473 g have been found in the predicted area. The first pieces were recovered on March 12, 2016 on a field close to the village of Stubenberg (Bavaria). Stubenberg is a weakly shocked (S3) fragmental breccia consisting of abundant highly recrystallized rock fragments embedded in a clastic matrix. The texture, the large grain size of plagioclase, and the homogeneous compositions of olivine (Fa(31.4)) and pyroxene (Fs(25.4)) clearly indicate that Stubenberg is an LL6 chondrite breccia. This is consistent with the data on O, Ti, and Cr isotopes. Stubenberg does not contain solar wind-implanted noble gases. Data on the bulk chemistry, IR spectroscopy, cosmogenic nuclides, and organic components also indicate similarities to other metamorphosed LL chondrites. Noble gas studies reveal that the meteorite has a cosmic ray exposure (CRE) age of 36 +/- 3 Ma and that most of the cosmogenic gases were produced in a meteoroid with a radius of at least 35 cm. This is larger than the size of the meteoroid which entered the Earth's atmosphere, which is constrained to <20 cm from short-lived radionuclide data. In combination, this might suggest a complex exposure history for Stubenberg.

Published
2017
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14. Triple F--a comet nucleus sample return mission

Author

Küppers, Michael, Keller, H. U., Kührt, E., A'Hearn, M. F., Altwegg, K., Bertrand, R., Busemann, H., Capria, M. T., Colangeli, L., Davidsson, B., Ehrenfreund, P., Knollenberg, J., Mottola, S., Rathke, A., Weiss, P., Zolensky, M., Akim, E., Basilevsky, A., Galimov, E., Gerasimov, M., Korablev, O., Lomakin, I., Marov, M., Martynov, M., Nazarov, M., Zakharov, A., Zelenyi, L., Aronica, A., Ball, A. J., Barbieri, C., Bar-Nun, A., Benkhoff, J., Biele, J., Biver, N., Blum, J., Bockelée-Morvan, D., Botta, O., Bredehöft, J. H., Capaccioni, F., Charnley, S., Cloutis, E., Cottin, H., Cremonese, G., Crovisier, J., Crowther, S. A., Epifani, E. M., Esposito, F., Ferrari, A. C., Ferri, F., Fulle, M., Gilmour, J., Goesmann, F., Gortsas, N., Green, S. F., Groussin, O., Grün, E., Gutiérrez, P. J., Hartogh, P., Henkel, T., Hilchenbach, M., Ho, T. M., Horneck, G., Hviid, S. F., Ip, W. H., Jäckel, A., Jessberger, E., Kallenbach, R., Kargl, G., Kömle, N. I., Korth, A., Kossacki, K., Krause, C., Krüger, H., Li, Z. Y., Licandro, J., Lopez-Moreno, J. J., Lowry, S. C., Lyon, I., Magni, G., Mall, U., Mann, I., Markiewicz, W., Martins, Z., Maurette, M., Meierhenrich, U., Mennella, V., Ng, T. C., Nittler, L. R., Palumbo, P., Pätzold, M., Prialnik, D., Rengel, M., Rickman, H., Rodriguez, J., Roll, R., Rost, D., Rotundi, A., Sandford, S., Schönbächler, M., Sierks, H., Srama, R., Stroud, R. M., Szutowicz, S., Tornow, C., Ulamec, S., Wallis, M., Waniak, W., Weissman, P., Wieler, R., Wurz, P., Yung, K. L., Zarnecki, J. C., Schonbachler, Maria, Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Solar System, Cosmic Vision, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], sample return, Sample return, space mission, 7. Clean energy, 01 natural sciences, Space mission, Astrobiology, Interplanetary dust cloud, Sample return mission, Comet nucleus, 0103 physical sciences, Comets, comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, Cosmogony, 13. Climate action, Space and Planetary Science, cosmogony, Formation and evolution of the Solar System, business
Abstract

The Triple F (Fresh From the Fridge) mission, a Comet Nucleus Sample Return, has been proposed to ESA's Cosmic Vision program. A sample return from a comet enables us to reach the ultimate goal of cometary research. Since comets are the least processed bodies in the solar system, the proposal goes far beyond cometary science topics (like the explanation of cometary activity) and delivers invaluable information about the formation of the solar system and the interstellar molecular cloud from which it formed. The proposed mission would extract three sample cores of the upper 50cm from three locations on a cometary nucleus and return them cooled to Earth for analysis in the laboratory. The simple mission concept with a touch-and-go sampling by a single spacecraft was proposed as an M-class mission in collaboration with the Russian space agency ROSCOSMOS. © The Author(s) 2008.

Published
2009

16. NEW TITANIUM ISOTOPE DATA FOR ALLENDE AND EFREMOVKA CAIs

Author

Leya, Ingo, Schonbachler, Maria, Krahenbuhl, Urs, and Halliday, Alex N.

Abstract

We measured the titanium (Ti) isotope composition, i.e., 50Ti/47Ti, 48Ti/47Ti, and 46Ti/47Ti, in five calcium-rich-aluminum-rich refractory inclusions (CAIs) from the oxidized CV3 chondrite Allende and in two CAIs from the reduced CV3 chondrite Efremovka. Our data indicate that CAIs are enriched in 50Ti/47Ti and 46Ti/47Ti and are slightly depleted in 48Ti/47Ti compared to normal Ti defined by ordinary chondrites, eucrites, ureilites, mesosiderites, Earth, Moon, and Mars. Some CAIs have an additional 50Ti excess of [?]8e relative to bulk carbonaceous chondrites, which are enriched in 50Ti by [?]2e relative to terrestrial values, leading to a total excess of [?]10e. This additional 50Ti excess is correlated with nucleosynthetic anomalies found in 62Ni and 96Zr, all indicating an origin from a neutron-rich stellar source. Bulk carbonaceous chondrites show a similar trend, however, the extent of the anomalies is either less than or similar to the smallest anomalies seen in CAIs. Mass balance calculations suggest that bulk Allende Ti possibly consists of a mixture of at least two Ti components, anomalous Ti located in CAIs and a normal component possibly for matrix and chondrules. This argues for a heterogeneous distribution of Ti isotopes in the solar system. The finding that anomalous Ti is concentrated in CAIs suggests that CAIs formed in a specific region of the solar system and were, after their formation, not homogeneously redistributed within the solar system. Combining the CAI data with improved model predictions for early solar system irradiation effects indicates that a local production scenario for the relatively short lived radionuclides can be excluded, because the production of, e.g., 10Be, 26Al, and 41Ca, would result in a significant collateral shift in Ti isotopes, which is not seen in the measured data.

Published
2009

17. Zirconium isotope heterogeneities in the solar system

Author

Akram, Waheed, Lyon, Ian, and Schonbachler, Maria

Subjects
523, Meteorites, Cosmochemistry, Zirconium, Neutron-capture, MC-ICP MS
Abstract

Laboratory measurements of primitive and differentiated meteorites have been made in order to understand the origin of isotopic anomalies. The element Zr is chosen for analysis, due to its potential for nuclear and astrophysical applications. Zirconium has five stable isotopes that are produced in different (neutron–capture) nucleosynthetic processes. By analysing the Zr isotope composition of meteorites, we are able to track the mixing of various neutron capture processes in the early Solar System. Measurements have been performed on carbonaceous, ordinary and enstatite chondrites, eucrites, the Moon and Earth. Samples are crushed, digested and passed through a two stage anion exchange separation to obtain a clean Zr fraction. All Zr measurements are made on a Nu Plasma multiple–collector inductively coupled plasma mass spectrometer (MC–ICPMS). The results indicate that the bulk of refractory Ca–Al rich inclusions of the Allende meteorite are characterised by uniform enrichments (around 2ε) of the neutron–rich isotope 96Zr, and potentially coupled with excesses reported for the neutron rich isotope 50Ti, indicating that both nuclides may have similar astrophysical origins. Analysis of bulk rock carbonaceous chondrites reveal 96Zr excesses (not exceeding 1ε) that scale with the abundance of CAIs. However, widespread 96Zr correlations are also seen, accompanied by minor depletions in 91Zr, which suggest the solar nebular had experienced thermal heating of some sort, altering the initial (possibly uniform) Zr isotope composition of the early Solar System from which planetary bodies formed.

Published
2013

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