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Dynamics and Energetics of Magnetic Activity in the Galactic Center

柿内, 健佑 名古屋大学

2023.06.26

概要

学位報告4

別紙4
報 告 番












論文題目











Dynamics and Energetics of Magnetic Activity in the Galactic Center
(銀河系中心領域の磁気活動についての理論的研究)













論 文 内 容 の 要 旨
宇宙空間には数多の銀河が存在する。銀河の構造とダイナミクスを解明は、現代天文学におけ
る重要な課題である。天の川銀河を含む主要な銀河の多くは渦巻銀河と呼ばれ、円盤部と中心部
からなる。特に、銀河の中心部には大量の恒星と星間ガスが集積し活発な天体現象が確認されて
いる。我々から最も近い銀河系の中心部ではその詳細な構造について観測が進んでいる。しかし、
中心部の複雑な状況を理解するためには銀河の重力場だけ説明が難しいことが分かってきた。
銀河系中心部数100パーセクにおける領域での磁場強度は円盤部に比べて強く、その磁気エ
ネルギーは星間ガスの熱・運動エネルギーに匹敵、あるいは凌駕する。本研究では、銀河系中心
領域における磁場の増幅とそれに伴うガスの密度構造や運動構造、エネルギー分布への影響につ
いて明らかにするために大局的磁気流体数値実験を用いて研究を行う。
申請者はまず、磁気活動によるガスの流れについて理解するために、すでに実施されていた大
局的磁気流体数値実験データを用いて星間ガスと磁場の相互作用によって引き起こされるガスの
流れについての詳細な解析を行った。その結果、パーカー(1966)で提唱された磁気浮上ガスによ
る鉛直方向にガスが持ち上げられ再度重力で加速される流れを発見した。この流れが視線方向に
重なることで非常に幅広い速度分散をもった構造に見えることを明らかにした。
次に、申請者は、磁場強度と熱・運動エネルギーの関係を理解するために、星間ガスの輻射加
熱冷却スキームを実装した数値シミュレーションを行なった。その結果、加熱冷却の有無によら
ず、磁場強度は平均で 10μG、最大で数 100μG に達した。これにより磁場増幅の飽和値は大局的
なダイナミクスで決まるという示唆を得た。輻射加熱冷却過程を考慮した結果として、銀河面の
温度は輻射加熱と冷却で決まる熱平衡曲線に従い約 104K になる。そして、銀河面と上空の中間領
域において、ガス圧に比べて磁気圧が非常に卓越する領域が確認された。一方、z/R > 1.0 の上空
には T = 107 K に達するような高温(コロナ)ガスが輻射加熱と磁気散𨓜による加熱よって形成
され得ることが分かった。

学位関係

上記の実験結果から申請者は銀河系中心領域においてガス圧に対する磁場強度によって決まる
z 方向の厚みが存在することを明らかにした。また、磁気圧優勢な領域では銀河面上空に向かって
ガス運動を活性化させ、特徴的なガスの運動や密度構造を形成することを突き止めた。

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