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大質量星形成の極初期段階における複雑な有機分子
酒井, 剛
Permalink : http://hdl.handle.net/2115/77789
JaLCDOI : 10.14943/lowtemsci.78.253
KEYWORDS : 大質量星形成;有機分子;星間分子;high-mass star formation;complex organic molecules;interstellar molecules
Abstract
大質量星（太陽の8倍以上の質量を持つ恒星）形成領域において原始星周囲の化学組成は，小質量 星形成領域のそれとは異なる点が見られる．特に，窒素を含む複雑な有機分子の存在量は大質量星形 成領域の方が多い．大型ミリ波サブミリ波干渉計ALMAを用い，大質量星形成の極初期段階にある 天体（G34.43＋00.24MM3）を観測したところ，窒素を含む複雑な有機分子の存在量が，他の比較的 進化の進んだ大質量星形成領域と同程度であることがわかった．このことは，大質量星形成において， 原始星周囲の化学組成は極初期から小質量星形成領域の化学組成と異なっていることを示している． 本稿では，重水素化分子などの存在量も踏まえ，大質量星形成領域の複雑な有機分子の起源について 議論する
The chemical compounds in high-mass protostars are different from those in low-mass protostars. For example, nitrogen-bearing complex organic molecules(N-bearing COMs),such as CH3CH2CN,are known to be more abundant in high-mass sources than in low-mass sources. We observed a very young protostar in a high-mass star-forming region (G34.43+00.24 MM3) and found that the abundance of CH3CH2CN in G34.43+00.24 MM3 is as high as that in other high-mass sources. In this paper, we discuss the origin of the COMs in high-mass star-forming regions.
The chemical compounds in high-mass protostars are different from those in low-mass protostars. For example, nitrogen-bearing complex organic molecules(N-bearing COMs),such as CH3CH2CN,are known to be more abundant in high-mass sources than in low-mass sources. We observed a very young protostar in a high-mass star-forming region (G34.43+00.24 MM3) and found that the abundance of CH3CH2CN in G34.43+00.24 MM3 is as high as that in other high-mass sources. In this paper, we discuss the origin of the COMs in high-mass star-forming regions.
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