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二重中性子星の合併による重力波に続く検出可能なラジオフレア
1Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel. udini@wise.tau.ac.il
Nature
|October 4, 2011
まとめ
中性子星の融合は重力波を作り,長時間続く電波フレアを生成する. これらのフレアは,周囲の物質と相互作用するアウトフローから発生し,これらの宇宙イベントの検出可能な電磁気シグネチャーを提供します.
科学分野:
- 天体物理学 天体物理学
- 引力波天文学 引力波天文学
- マルチメッセンジャー天文学
背景:
- 中性子星の合併は重力波の主要な源である.
- これらの合併は,アウトフローを起動し,短時間のガンマ線爆発を潜在的に説明することができます.
- 永続的な電磁気シグネチャーは,重力波の検出を確認するために不可欠です.
研究 の 目的:
- 中性子星の合併による流出の電磁気シグネチャーを調査するために.
- これらのアウトフローが検出可能な無線フレアを生成できるかどうかを判断するために.
- 観測された無線トランジエントと中性子星の融合を関連付ける.
主な方法:
- 相対論的流出と周囲の媒体の相互作用に関する計算を行った.
- 様々な周波数 (150MHz,1.4GHz) のモデルのラジオフレア放射.
- 異なる赤偏移でのフレアの持続時間と検出度を分析した.
主要な成果:
- 軽度の相対論的アウトフローは,0.1.1の赤色シフトまで,数週間の間,1.4GHzで検出可能な無線フレア (サブミリヤンスキー) を生成します.
- 亜相対性流出は,150MHzと1.4GHzで長年にわたって検出可能なフレアを生成します.
- ラジオトランジントRT 19870422は,中性子星の合併による流出の予測された性質と一致します.
結論:
- 中性子星の融合による流出は,観測可能なラジオフレアを生成します.
- これらのフレアは,重力波のイベントに潜在的電磁対照を提供する.
- このモデルは,RT 19870422が中性子星の合併から生じたと説明しています.
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