Mostrando 21 - 40 Resultados de 59 Para Buscar 'protoplaneta*', tiempo de consulta: 0.21s Limitar resultados
  1. 21
    por Nguyen, Ann N., Mane, Prajkta, Keller, Lindsay P., Piani, Laurette, Abe, Yoshinari, Aléon, Jérôme, Alexander, Conel M. O'D., 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, 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, Itoh, Shoichi, Kawasaki, Noriyuki, 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, Frédéric, Nakai, Izumi, Nagashima, Kazuhide, Nesvorný, David, Nittler, Larry, Onose, Morihiko, Pack, Andreas, Park, Changkun, Qin, Liping, Russell, Sara S., Sakamoto, Naoya, Schönbächler, 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
    Publicado 2023
    “…The 5 to 10 times higher abundances of presolar SiC (~235 ppm), N-rich organic matter, organics with N isotopic anomalies (1.2%), and organics with C isotopic anomalies (0.2%) in the primitive clasts compared to bulk Ryugu suggest that the clasts formed in a unique part of the protoplanetary disk enriched in presolar materials. These clasts likely represent previously unsampled outer solar system material that accreted onto Ryugu after aqueous alteration ceased, consistent with Ryugu’s rubble pile origin.…”
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    Abundant presolar grains and primordial organics preserved in carbon-rich exogenous clasts in asteroid Ryugu
  2. 22
    “…Transport of olivine within the Solar System probably occurred also due to protostellar jets and winds but the entrainment in SBSS from interstellar space would overcome the requirement of initial turbulent regime in the protoplanetary nebula.…”
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    Igneous processes in the small bodies of the Solar System I. Asteroids and comets
  3. 23
    “…Terrestrial and sub-Neptune planets are expected to form in the inner (less than 10 au) regions of protoplanetary disks(1). Water plays a key role in their formation(2–4), although it is yet unclear whether water molecules are formed in situ or transported from the outer disk(5,6). …”
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    Water in the terrestrial planet-forming zone of the PDS 70 disk
  4. 24
    “…Here we demonstrate that the current data clearly indicate spatial heterogeneity of (26)Al by a factor of 3-4 in the precursor molecular cloud or the protoplanetary disk of the Solar System, likely associated with the late infall of stellar materials with freshly synthesized radionuclides.…”
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    Igneous meteorites suggest Aluminium-26 heterogeneity in the early Solar Nebula
  5. 25
    “…This gas will contain only traces of elements like C, N and O, because those elements have frozen out as ices. ProDiMo protoplanetary disk models are used to predict the chemical evolution of gas and ice in the midplane. …”
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    Disk Evolution, Element Abundances and Cloud Properties of Young Gas Giant Planets
  6. 26
    “…The amount of gas that has been captured from the protoplanetary disk into the planetary atmosphere is calculated by solving the hydrostatic structure equations in the protoplanetary nebula. …”
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    Escape of the martian protoatmosphere and initial water inventory
  7. 27
    “…These results strongly suggest that both the formation of chondritic refractory organics and the trapping of noble gases took place simultaneously in the ionized areas of the protoplanetary disk, via photon- and/or electron-driven reactions and processing. …”
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    Synthesis of refractory organic matter in the ionized gas phase of the solar nebula
  8. 28
    “…Overall, the high abundance of COMs in cometary ices supports the formation through grain-surface reactions in the solar system protoplanetary disk.…”
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    Ethyl alcohol and sugar in comet C/2014 Q2 (Lovejoy)
  9. 29
    “…Collectively, these observations suggest that the CV chondrules formed from precursors that originated in various regions of the protoplanetary disk and were then transported to the accretion region of the CV parent asteroid whereas CR chondrule predominantly formed from precursor with carbonaceous chondrite-like μ(54)Cr signatures. …”
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    Magnesium and (54)Cr isotope compositions of carbonaceous chondrite chondrules – Insights into early disk processes
  10. 30
    “…Based on the small masses and sizes of their protoplanetary disks3,4, core-accretion theory for ultracool dwarfs predicts a large, but heretofore undetected population of close-in terrestrial planets5, ranging from metal-rich Mercury-sized planets6 to more hospitable volatile-rich Earth-sized planets7. …”
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    Temperate Earth-sized planets transiting a nearby ultracool dwarf star
  11. 31
    “…The diversity of primitive particles has implications for the diversity of materials in the protoplanetary disc present at the time and in the region where the comets formed. …”
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    Cometary dust: the diversity of primitive refractory grains
  12. 32
    “…This finding is consistent with a primary chondrule formation episode during the early high-mass accretion phase of the protoplanetary disk that transitions into a longer period of chondrule reworking. …”
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    Early formation of planetary building blocks inferred from Pb isotopic ages of chondrules
  13. 33
    “…Since this organic carbon thermally decomposes above ∼450 K, GEMS cannot have accreted in the hot solar nebula, and formed, instead, in the cold presolar molecular cloud and/or outer protoplanetary disk. We suggest that GEMS are consistent with surviving interstellar dust, condensed in situ, and cycled through multiple molecular clouds.…”
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    Multiple generations of grain aggregation in different environments preceded solar system body formation
  14. 34
    “…Based on physical modeling of condensation within the protoplanetary disk, we attribute these isotopic compositions to the rapid condensation of AOAs over timescales of days to weeks. …”
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    Rapid condensation of the first Solar System solids
  15. 35
    “…Planet formation is generally described in terms of a system containing the host star and a protoplanetary disk(1–3), of which the internal properties (for example, mass and metallicity) determine the properties of the resulting planetary system(4). …”
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    Stellar clustering shapes the architecture of planetary systems
  16. 36
    “…We also address the associated processes of outflow launching and the formation of multiple systems, and discuss possible implications in properties of protoplanetary disks.…”
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    Formation and Evolution of Disks Around Young Stellar Objects
  17. 37
    por Ganino, Clément, Libourel, Guy
    Publicado 2020
    “…None have been yet applied to pristine asteroids formed in the solar protoplanetary disk, mainly because of their comminution during their 4.5-billion-year collisional lifetime. …”
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    Fumarolic-like activity on carbonaceous chondrite parent body
  18. 38
    por Ku, Y., Jacobsen, S. B.
    Publicado 2020
    “…Thus, the heterogeneous distribution of both refractory and moderately volatile elements in chondritic meteorites points to a limited radial mixing in the protoplanetary disk.…”
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    Potassium isotope anomalies in meteorites inherited from the protosolar molecular cloud
  19. 39
    “…However, the location of CO self-shielding (molecular cloud or protoplanetary disk) remains unknown. Here we show that CAIs with predominantly low ((26)Al/(27)Al)(0), <5 × 10(−6), exhibit a large inter-CAI range of Δ(17)O, from −40‰ to −5‰. …”
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    Oxygen isotopic heterogeneity in the early Solar System inherited from the protosolar molecular cloud
  20. 40
    “…They formed in the hot inner protoplanetary disk and, as such, provide insights into the earliest disk dynamics and physicochemical processing of the dust and gas that accreted to form the Sun and its planetary system. …”
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    Episodic formation of refractory inclusions in the Solar System and their presolar heritage
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