集積する中性子星によって電力を供給される超光るX線源

M Bachetti¹, F A Harrison², D J Walton²

¹1] Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France [2] CNRS, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France.

Nature

|October 10, 2014

まとめ

超明るいX線源は,しばしばブラックホールと考えられ,磁気化された中性子星である可能性があります. これらの発見は,コンパクトな物体への蓄積の現在のモデルに挑戦しています.

科学分野:

天体物理学天体物理学
高エネルギー天体物理学
X線天文学X線天文学とは

背景:

超光X線源 (ULXs) は,恒星質量ブラックホールのエディントン限度を超えています.
理論的なモデルは,質量要件のためにULXのブラックホールシステムを好む.
最も明るく輝くULX (> 10^40 ergs/sec) を説明するには,巨大なブラックホールまたは非標準の蓄積が必要である.

研究の目的:

超光X線源の性質を調査する.
中性子星がULX群に寄与できるかどうかを判断する.
蓄積物理学の既存のモデルに挑戦し,精錬する.

主な方法:

M82銀河の核領域のブロードバンドX線観測.
脈動とX線放射のシヌソイド変調の分析.
脈動性および可変性X線源の空間的偶然分析.

主要な成果:

M82.82の源から脈動 (1.37秒周期) と二次変調 (2.5d周期) の発見
パルス流は,4.9 × 10^39 ergs/sec (3-30 keV) の光度を示しています.
源は1.8 × 10^40 ergs/sec (0.3-10 keV) に達し,太陽質量1.4の中性子星のエディントン限界の約100倍である.

結論:

磁性中性子星は,超光るX線源である可能性があります.
この発見は,ULXがブラックホールシステムのみであるという仮定に異議を唱える.
観測された明るさは,中性子星がULXの間で一般的である可能性を示唆し,蓄積モデルの限界を押し広げます.

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