@article{oai:miyazaki-u.repo.nii.ac.jp:00002385,
 author = {園田, 絵里 and Sonoda, Eri and 山内, 誠 and Yamauchi, Makoto and 前野, 将太 and Maeno, Shouta and 山本, 幹生 and Yamamoto, Mikio and 松尾, 嘉比古 and 河合, 誠之 and Kawai, Nobuyuki and 小浜, 光洋 and Kohama, Mitsuhiro and 園田, 絵里 and Sonoda, Eri and 前野, 将太 and Maeno, Shouta and Matsuo, Yoshihiko and 河合, 誠之 and Kawai, Nobuyuki and 小浜, 光洋 and Kohama, Mitsuhiro},
 journal = {宮崎大学工学部紀要, Memoirs of Faculty of Engineering, University of Miyazaki},
 month = {Aug},
 note = {GRB041006 was first detected by HETE-2 on 2004 Oct. 6 at 12:18:08 UT. We have
observed it's earliest optical afterglow from 12:19:18 UT to through the night. Our
observation was performed by using the unfiltered CCD camera on the 30-cm telescope. We
combined our converted R band data with those reported by GCN. Statistics don't allow us to
say in detail but the light curve shows two slope changes. The power-low index α of the
flux decay is α =0.62 before about 0.0053 day after the burst, α =-0.45 from 0.0053 day to
0.077 day after the burst, and α =-1 after 0.077 day. These index changes can be explained
by forward shock in synchrotron shock model. During the first flat period, optical emission is
generated by cooling of all electrons, which are accelerated by forward shock. But the speed
of the shell become slower, then the critical frequency becomes lower than the optical band.
The light curve, therefore, got dark slowly. And finally, since the minimum frequency at
which the slowest ones among the accelerated electrons emit is below the optical frequency,
the electrons that can emit optical light decrease rapidly. So the afterglow darkened fast.},
 pages = {15--21},
 title = {RIMOTSによるGRB041006の可視光残光の早期観測},
 volume = {34},
 year = {2005},
 yomi = {ソノダ, エリ and ヤマウチ, マコト and マエノ, ショウタ and ヤマモト, ミキオ and マツオ, ヨシヒコ and カワイ, ノブユキ and コハマ, ミツヒロ and ソノダ, エリ and マエノ, ショウタ and カワイ, ノブユキ and コハマ, ミツヒロ}
}