Zobrazeno 1 - 10
of 10
pro vyhledávání: '"光学的厚さ"'
Autor:
Machida, Ryosuke, Abe, Yutaka
Publikováno v:
第40回月・惑星シンポジウム = Proceedings of the 40th ISAS Lunar and Planetary Symposium. :177-180
資料番号: AA0063723040
Autor:
Machida, Ryosuke, Abe, Yutaka
Publikováno v:
第39回月・惑星シンポジウム = Proceedings of the 39th ISAS Lunar and Planetary Symposium. :162-165
資料番号: AA0063505042
Autor:
Suzuki, Makoto, Okumura, Shinichiro, Yoshida, Shigeomi, Watanabe, Masaharu, Imamura, Takeshi, Nakamura, Masato, Kita, Kazuyuki, Takahashi, Yukihiro, Ushio, Tomoo
Publikováno v:
第5回宇宙科学シンポジウム = Proceedings of the 5th Space Science Symposium. :360-363
資料番号: AA0049122089
Publikováno v:
第5回宇宙科学シンポジウム = Proceedings of the 5th Space Science Symposium. :611-614
VSOP(VLBI Space Observatory Programme)とVLBA(VLBI Array)を用いて1.6-15.4GHzの5周波で18天体のGHz-Peaked Spectrum(GPS)電波源のサーベイ観測を行なった結果を報告する。GPS電波源はGHz帯にピークを持つ連続ス
Publikováno v:
大気圏シンポジウム第18回 平成15年度 = Atmospheric Science Symposium the 18th 2003. :30-33
資料番号: AA0046920009
Publikováno v:
第37回月・惑星シンポジウム = Proceedings of the 37th ISAS Lunar and Planetary Symposium. :208-211
It has been proposed that warm and wet climate was induced on early Mars by the scattering greenhouse effect of CO2 ice clouds. However, such clouds receive strong infrared heating in warm atmosphere and might evaporate before causing sufficient gree
Autor:
Sato, Yasuhiko, Kawabata, Kiyoshi
Publikováno v:
第36回月・惑星シンポジウム = Proceedings of the 36th ISAS Lunar and Planetary Symposium. :210-213
In order to study the influence of a lower layer of Venus atmosphere, the mode 3 particle which is not incorporated into calculation has been introduced. For this purpose, multiple scattering computations of the incident sunlight are carried out usin
Publikováno v:
京都大学防災研究所年報. B. 46:503-515
気象モデルと連結したエアロゾルモデルシステム(MSSP:Regional Eulerian ModelSystem for Soluble Particles) を構築した。MSSPは酸性雨,雲物理,領域的寒冷化などに大きく寄与する水溶性エアロゾルを
Autor:
Sasaki, Sho
Publikováno v:
第28回月・惑星シンポジウム = Proceedings of the 28th ISAS Lunar and Planetary Symposium. :221-224
Dust ejection efficiency from Phobos/Deimos controls dust abundance of Martian dust torus. Martian oblateness effect together with solar radiation pressure enhances abundance of particles with radius 20-200 micrometer of Phobos' dust torus. This is c
Publikováno v:
第28回月・惑星シンポジウム = Proceedings of the 28th ISAS Lunar and Planetary Symposium. :25-28
資料番号: AA0063352007