茶色矮星ディスクにおける惑星形成の始まり
Dániel Apai1, Ilaria Pascucci, Jeroen Bouwman
1Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA. apai@as.arizona.edu
まとめ
塵の成長と沈着を含む惑星形成プロセスは,茶色矮星の周りの冷たい円盤で起こり,星の周りのものと似ています. これは,惑星の形成が若い環恒星円盤における一般的なプロセスであることを示唆しています.
科学分野:
- 天文学と天体物理学について
- エクソプラネット科学 エクソプラネット科学
背景:
- 惑星の形成は,塵の粒が成長し,原惑星円盤に定着することから始まります.
- これらのプロセスは,低質量および中質量恒星の周りの円盤でよく研究されています.
研究 の 目的:
- 茶色矮星の周りの円盤の惑星形成過程を調査する.
- 茶色矮星円盤の塵の進化を恒星円盤と比較するために.
主な方法:
- 茶色矮星と候補星周辺のディスクからの赤外線スペクトルの取得と分析.
- 観測されたスペクトル特性の比較と,塵の成長と沈着のモデル.
主要な成果:
- 赤外線スペクトルは,粉塵の成長と茶色矮星周辺のディスクに沈着することを明らかにします.
- これらのプロセスは,恒星の周りの円盤で観察されたものと類似または同一です.
結論:
- 惑星形成の始まりは,茶色矮星の周りの冷たい円盤で起こります.
- 惑星の形成は,中心物体の質量に関係なく,ほとんどの若い周周円盤に共通する堅固なプロセスです.
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