[論文レビュー] Magnetic field detections in massive systems at different stages of interaction

S. Hubrig, M. Abdul-Masih+5 more|arXiv (Cornell University)|Jan 18, 2026

Astrophysics and Star Formation Studies被引用数 0

ひとこと要約

研究は14の大質量連星/多重系の53件の高分解能分光偏光観測を分析し、SV Cenのみ僅かな検出に留まる以外はすべて磁場を検出、磁場強度は数百ガウスから数キロガウスまでと推定され、系成分間の相互作用が磁場生成に寄与していることを示唆する。

ABSTRACT

Despite the importance of magnetic fields in massive stars, their origin is widely debated and still not well understood. With the mounting evidence for the importance of studying magnetic fields in interacting massive binary and multiple systems, it appears necessary to investigate the presence of magnetic fields in semi-detached systems with ongoing mass transfer, and in contact systems where mass is actively being exchanged. We present an analysis of 53 high-resolution HARPSpol spectropolarimetric observations of a sample of 14 massive binary and multiple systems using the least-squares deconvolution technique. The majority of the studied systems are classified as semi-detached or contact binaries. Definite detections of the presence of a magnetic field are achieved in all studied systems apart from the rather faint system SV Cen, for which only a marginal detection was obtained. The fact that the presence of magnetic fields is detected in all but one of the studied systems strongly suggests that interaction between the system components plays a definite role in the generation of magnetic fields in massive stars. The measured mean longitudinal magnetic field strength for all targets is of the order of a few hundred Gauss to a few kiloGauss. The strongest longitudinal magnetic fields of 4 to 5kG are discovered in the massive O-type triple system MY Ser in both components of the contact binary. kiloGauss-order magnetic fields are also detected in two other systems, V1294 Sco and V606 Cen. It is possible that there is an implication of some system characteristics, such as multiplicity, the mass ratio between the components, and a large fillout factor, on the measured magnetic field strength. Our results for the magnetic field measurements in interacting binaries present the first assessment of the occurrence rate of magnetic fields in a representative sample of such systems.

研究の動機と目的

• 質量移動が進行中のsemi-detachedおよびcontact大質量連星/多重系に磁場が存在するかを調査する。
• 磁場と系の相互作用段階および多重性、質量比、充填因子などの構造パラメータとの相関を評価する。
• 相互作用する大系の代表サンプルにおける磁場発生の Occurrence Rate の初めての評価を提供する。

提案手法

• 53件の高分解能HARPSpol分光偏光観測を分析する。
• 磁場を検出するために最小二乗デコンvolution法を適用する。
• ターゲット全体で平均縦磁場強度を測定する。

実験結果

リサーチクエスチョン

• RQ1 大質量の相互作用連星・多重系は、質量移動または接触相において検出可能な磁場を示すか。
• RQ2 これらの系で典型的な磁場強度はどのくらいで、系の特性とどう関連するか。
• RQ3 半分離/接触構成全体で磁場の存在は普遍的か、それともいくつかの系は例外か。

主な発見

• 研究対象の全系でSV Cenを除き磁場を検出（SV Cenは検出が僅か）。
• 平均縦磁場強度は通常数百ガウスから数キロガウスの範囲。
• 最も強い磁場（4–5 kG）はO型トリプルMY Serの接触構成にある両成分で検出。
• V1294 ScoおよびV606 Cenでもキロガウス級の磁場を検出。
• 系の相互作用特性が磁場強度と発生に影響を与える可能性が示唆される。