@inproceedings{oai:jaxa.repo.nii.ac.jp:00020466,
 author = {三浦, 均 and 中本, 泰史 and 土居, 政雄 and Miura, Hitoshi and Nakamoto, Taishi and Doi, Masao},
 book = {第39回月・惑星シンポジウム, Proceedings of the 39th ISAS Lunar and Planetary Symposium},
 month = {Aug},
 note = {Millimeter-sized, spherical silicate grains abundant in chondritic meteorites, which are called as chondrules, are considered to be a strong evidence of the melting event of the dust particles in the protoplanetary disk. One of the most plausible scenarios is that the chondrule precursor dust particles are heated and melt in the high-velocity rarefied gas flow (shock-wave heating model). We considered the deformation of rotating molten dust particles exposed to the gas flow by using the three-dimensional hydrodynamic simulation. It is assumed that the viscosity of the droplet is so high that the droplet cannot deform within the rotation time scale. We found that under a certain condition, the droplet deforms to a prolate shape and its shape is very similar to the prolate chondrules measured by Tsuchiyama et al. (2003). Our results strongly suggest that once-melted precursor particles of such prolate chondrules have solidified in the high-velocity gas flow with a proper rotation rate., 資料番号: AA0063505004},
 pages = {13--16},
 publisher = {宇宙航空研究開発機構宇宙科学研究本部, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS)},
 title = {Shock-wave heating model for chondrule formation: Formation of prolate chondrules},
 year = {2006}
}