ノヴァ・デルフィニ2013の膨張する火球

G H Schaefer¹, T ten Brummelaar¹, D R Gies²

¹The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, California 91023, USA.

Nature

|November 4, 2014

まとめ

2013年のノヴァ・デルフィニの初期の観測は,近赤外線干渉測定を用いてその構造を明らかにした. この研究は,白矮星での熱核の脱走後に急速に発達する双極形状を示唆しています.

科学分野:

天文学天文学
天体物理学天体物理学
恒星の進化について

背景:

クラシックな新星は,二重星系における白矮星の蓄積における熱核の脱走の結果である.
遅い段階のエジェクタ構造は,共通エンベロープの相互作用または固有の双極性爆発から生じることがあります.
初期段階の新星構造の研究は,必要な高い空間解像度のために困難です.

研究の目的:

ノヴァ・デルフィニ2013の初期段階の構造と拡大を調査する.
ノバ・デルフィニ2013の角拡大と放射速度を用いて,その距離を決定する.

主な方法:

ノバ・デルフィニ2013の角度尺度の近赤外線インターフェロメトリック測定,爆発後1日目から開始.
最初の43日間の継続的なモニタリングで,見かけの膨張率の変化を追跡します.
角膨張データと放射速度測定を組み合わせて距離を測定する.

主要な成果:

膨張速度の観測された変化は,光学的に厚いコアと拡散封筒のモデルと一致しています.
光分布の円性が検出され,2日目には前立体または二極構造を示した.
ノヴァ・デルフィニ2013の幾何学的な距離は4.54 ± 0.59キロパルセックであった.

結論:

ノヴァ・デルフィニ2013は,進化の初期に双極構造を示した.
膨張しているエジェクトの光学的深さは,分散するにつれて変化します.
導出された距離は,この古典的な新星現象を理解するための重要なパラメータを提供します.

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