Departmental Bulletin Paper 若い中質量星周りの原始惑星系円盤の中間赤外撮像

本田, 充彦  ,  Honda, Mitsuhiko  ,  Maaskant, Koen  ,  岡本, 美子  ,  Okamoto, Yoshiko K.  ,  片坐, 宏一  ,  Kataza, Hirokazu  ,  山下, 卓也  ,  Yamashita, Takuya  ,  宮田, 隆志  ,  Miyata, Takashi  ,  酒向, 重行  ,  Sako, Shigeyuki  ,  藤吉, 拓哉  ,  Fujiyoshi, Takuya  ,  左近, 樹  ,  Sakon, Itsuki  ,  藤原, 英明  ,  Fujiwara, Hideaki  ,  上塚, 貴史  ,  Kamizuka, Takafumi  ,  Mulders, Gijs D.  ,  Lopez-Rodriguez, Enrique  ,  Packham, Christpher  ,  井上, 昭雄  ,  Inoue, Akio K.  ,  尾中, 敬  ,  Onaka, Takashi

26pp.23 - 31 , 2015-06-30 , 神奈川大学総合理学研究所
We imaged circumstellar disks around 22 Herbig Ae/Be stars at 25 μm using Subaru/COMICS and Gemini/T-ReCS. Our sample consisted of 11 group I (flaring disk) andgroup II (flat disk) sources. We found that group I sources tended to show more extended emission than group II sources. Previous studies showed that the continuous disk is hard to resolve with 8-meter-class telescopes in the Q-band due to the strong emissions from the unresolved innermost region of the disk. This indicates that Q-band resolution sources requires a hole orgap in the disk material distribution to suppress the contribution from the innermost region of the disk. As many group I sources are resolved at 25 μm, we suggest that many, not all, group I Herbig Ae/Be disks have a hole or gap and are (pre-)transitional disks. On the other hand, the unresolved nature of many group II sources at 25 μm supports the suggestion that group II disks have a continuous, flat disk geometry. It has been inferred that group I disks may evolve into group II through the settling of dust grains at the mid-plane of the proto-planetary disk. However, considering growing evidence of the presence of a hole or gaps in the disk of group I sources, such an evolutionary scenario is unlikely. The difference between groups I and II may reflect different evolutionary pathways of protoplanetary disks..
原著2014 年度神奈川大学総合理学研究所共同研究助成論文

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