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NGC 188の青い落後者にとって76%の二重星分数と異常な軌道パラメータがあります

Robert D Mathieu¹, Aaron M Geller

¹Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, Wisconsin 53706, USA. mathieu@astro.wisc.edu

|December 25, 2009

まとめ

ほとんどのブルー・ストラグラー・スターは二重星系に存在しており,その異常な明るさと質量増加は複数の星系内の相互作用によるものであることを示唆している. この発見は,それらの形成経路を解明するのに役立ちます.

科学分野:

星の天体物理学星の天体物理学
バイナリー・スター・システムバイナリー・スター・システム
スター・クラスター・ダイナミクス

背景:

ブルー・ストラグラー星は,恒星群の恒星群の中で,異常な明るさを持つメインシーケンス星である.
彼らの存在は,恒星の進化の標準的なモデルに異議を唱え,彼らは巨人または白矮星に進化したはずである.
以前の研究では,形成メカニズムとしてバイナリ相互作用が示唆されていたが,具体的なプロセスは不明であった.

研究の目的:

オープンな星団NGC188.8の青い落とし子星のバイナリー周波数を調査する.
ブルー・ラグラーが多星系から主として発生しているかどうかを判断する.
ブルー・ラグラーズの形成メカニズムと進化の経路を制限する.

主な方法:

NGC 188星団の青い落とし子星のフォトメトリックとスペクトル観測.
特定されたブルー・ストラグラー・バイナリーの軌道パラメータ (周期,離心率) の分析.
青い滞留星と通常のメインシーケンス星間のバイナリー周波数と恒星回転速度の比較.

主要な成果:

NGC 188の観測された青い落とし星のうち76%は二重星系に属しており,これは普通の星よりも3倍高い割合です.
これらのブルー・ストラグラー・バイナリは,明確な周期偏心分布を示しており,そのほとんどは約1,000日周期を有する.
青い落後星は,同様の温度を持つメインシーケンス星と比較して,より速い回転率を示しています.

結論:

高バイナリー周波数は,青い滞留星が多星系から形成されていることを強く支持しています.
質量移転,合併,双星内の恒星衝突は,おそらく同時形成プロセスである.
急速な回転は,青い落とし子に年齢制限を課し,その進化の軌跡に影響を与える可能性があります.

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