University of Tsukuba Center for Computational Sciences
University of Tsukuba Center for Computational Sciences
出版者
宇宙航空研究開発機構宇宙科学研究本部
出版者（英）
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS)
雑誌名
第37回月・惑星シンポジウム
雑誌名(英)
Proceedings of the 37th ISAS Lunar and Planetary Symposium
ページ
45 - 48
発行年
2004-02
抄録（英）
The existence of chondrules indicates that there were heating events of dust particles in the solar nebula. The shock-wave heating model is one of the most plausible models to explain the formation of chondrules. There are various studies of chondrule formation in a framework of the shock-wave heating model in the assumption of homogeneous temperature in dust particles. However, in the shock-wave heating, dust particles are heated from the surface by the gas friction heating, and the thermal energy is transferred toward the inside of the dust particles due to the thermal conduction. So it is expected that dust particles have inhomogeneous temperature distribution. Numerically simulated is whether this inhomogeneous distribution reveals or not. It was found that dust particles have inhomogeneous temperature distribution. For example, when the radius of dust particle is 1 mm, the maximum difference of temperature between the front and the back of the dust particle reaches about 300 K. In addition, for r(sub s) less than 450 micrometer, the back of dust particle does not melt under the condition of the shock velocity v(sub s) = 10 km/s and the post-shock density n(sub g) = 5.0 x 10(exp 14) cm(exp -3), with which condition the dust particles completely melt in the assumption of homogeneous temperature distribution, though the rest of the particle melts.
Inhomogeneous temperature distribution in chondrules in the shock-wave heating
