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ASASSN-18aan: An Eclipsing SU UMa-type Cataclysmic Variable with a 3.6-hour Orbital Period and a Late G-type Secondary Star

Wakamatsu, Yasuyuki 京都大学 DOI:10.14989/doctor.k23014

2021.03.23

概要

矮新星は主星とそれを取り巻く円盤、そして伴星からなる近接連星系である。矮新星のサブグループであるSU UMa型矮新星はスーパーアウトバーストと呼ばれる大規模な増光を起こす。スーパーアウトバーストの発生機構を説明するモデルとして広く受け入れられているのが潮汐不安定性モデルである。潮汐不安定性モデルでは、円盤外縁部が3:1共鳴半径まで広がり、潮汐不安定性によって円盤が離心楕円形に変形することによって、伴星の潮汐トルクにより効果的に角運動量が引き抜かれることでスーパーアウトバーストに発展すると考えられている。しかし、数値計算や流体計算の結果から、主星の周囲には共鳴半径とは別に、伴星の潮汐トルクによって円盤の広がりが制限される半径(tidal truncation radius)が存在することが知られている。スーパーアウトバーストは円盤が共鳴半径まで広がることができる時、すなわち3:1共鳴半径がtidal truncation radiusよりも小さい時に発生すると考えられている。これは、主星に対する伴星の質量比が0.25程度より小さいときに実現される。しかし、矮新星の中には質量比が0.25を大きく超えているにもかかわらずスーパーアウトバーストを起こしている可能性のあるものが存在することが知られている。また、WZ Sge型矮新星と呼ばれるより質量比の小さい天体の中には、円盤外縁部がtidal truncation radiusを超えて広がる可能性が観測的に示唆されているものもある。このようなこ とから、tidal truncation radiusが本当に円盤の広がりを止められるのかどうか、また、どのような条件では止められないのかについてはよくわかっていない。これを調べるためには、質量比が大きく、かつ伴星による円盤の食が起きる天体を観測するのが適している。これは、食の観測から円盤半径を見積もることができるためである。

本研究では、軌道周期の長いSU UMa型矮新星ASASSN-18aanのスーパーアウトバーストの集中的な観測を行った。標準的な進化経路を考えると、軌道周期が長い天体ほど質量比も大きく、実際、この観測からASASSN-18aanの質量比を見積もると0.278であった。今回、食の解析に際して新たな手法を開発して適用し、軌道傾斜角や円盤半径などのパラメータを推定に成功した。この結果から、ASASSN-18aanのスーパーアウトバーストの挙動も潮汐不安定性モデルで説明できるという結果が得られた。また、他の天体の調査から、SU UMa型矮新星のような質量比の比較的大きい天体では円盤の広がりはtidal truncation radiusで止められるが、WZ Sge型矮新星のような質量比の小さな系では円盤の広がりが止められないことを示唆する結果を得た。

さらに、ASASSN-18aanの伴星は同程度の軌道周期を持つ他の天体とは異なり、極めて温度が高いことが判明した。分光観測の結果からは、伴星のスペクトルには通常より強いナトリウムの吸収線が存在することがわかった。これは、伴星が主星への質量輸送を開始した時点で水素燃焼がかなり進んでいたことを意味し、ASASSN-18aanはいくつか知られている、伴星が異様に温かい矮新星の一つであるという結果が得られ た。

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