Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm

Takasao, Shinsuke; Kunitomo, Masanobu; Suzuki, K. Takeru; Iwasaki, Kazunari; Tomida, Kengo

doi:https://doi.org/10.3847/1538-4357/ada364

Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm

Takasao, Shinsuke; Kunitomo, Masanobu; Suzuki, K. Takeru et al.

The Astrophysical Journal, 2025, 980(1), 111

アクセス数:529件（2026-02-15 19:31 集計）

固定URL: https://hdl.handle.net/11094/100435

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タイトル	Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm
著者	NRID 1000090794727 1000090794727 ORCID 0000-0003-3882-3945 0000-0003-3882-3945 researchmap permalink shinsuke_takasao shinsuke_takasao Scopus Author ID 54891792200 54891792200 著者名 Takasao, Shinsuke
	NRID 1000020794621 1000020794621 著者名 Kunitomo, Masanobu
	NRID 1000080431782 1000080431782 著者名 Suzuki, K. Takeru
	NRID 1000050750379 1000050750379 著者名 Iwasaki, Kazunari
	NRID 1000070772367 1000070772367 著者名 Tomida, Kengo
内容	Takasao Shinsuke, Kunitomo Masanobu, Suzuki Takeru K., et al. Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm. The Astrophysical Journal 980, 111 (2025); https://doi.org/10.3847/1538-4357/ada364.
抄録	Stellar spin is one of the fundamental quantities that characterize a star itself and its planetary system. Nevertheless, stellar spin-down mechanisms in protostellar and pre-main-sequence stellar phases have been a long-standing problem in star formation theory. To realize the spin-down, previous axisymmetric models based on the conventional magnetospheric paradigm have had to assume massive stellar winds or produce highly time-variable magnetospheric ejections. However, this picture has been challenged by both numerical simulations and observations. With a particular focus on the propeller regime for solar-mass stars, we propose a new picture of stellar spin-down based on our recent 3D magnetohydrodynamic simulation and stellar evolution calculation. We show that failed magnetospheric winds, unique to 3D models, significantly reduce the spin-up accretion torque, which make it easier for the star to spin-down. Additionally, the amplitude of time variability associated with magnetospheric ejections is reduced by 3D effects. Our simulation demonstrates that the star spins down by generating a conical disk wind, driven by a rotating stellar magnetosphere. Our theoretical estimates, inspired by the numerical model, suggest that the conical disk wind is likely to play a crucial role in extracting stellar angular momentum during the protostellar phase. As magnetospheric accretion is expected to occur in other accreting objects such as protogiant planets, this study will also contribute to the understanding of the angular momentum of such objects.
出版者	American Astronomical Society
収録物名	The Astrophysical Journal
巻(号)	980(1)
ページ	111
刊行年月	2025-02-10
言語	英語
ハンドルURL	https://hdl.handle.net/11094/100435
PISSN	0004637X
eISSN	15384357
関連情報 (isIdenticalTo)	DOI (出版社版) https://doi.org/10.3847/1538-4357/ada364
アクセス権	open access
権利情報	This article is licensed under a Creative Commons Attribution 4.0 International License.
出版タイプ	Version of Record
カテゴリ	学術雑誌論文 Journal Article

資源タイプ	学術雑誌論文
ローカル資源タイプ	学術雑誌論文
DCTERMS.bibliographicCitation	The Astrophysical Journal. 2025, 980(1), p. 111
DC.title	Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm
DC.creator	Takasao, Shinsuke
	Kunitomo, Masanobu
	Suzuki, K. Takeru
	Iwasaki, Kazunari
	Tomida, Kengo
DC.publisher	American Astronomical Society
DC.language' scheme='DCTERMS.RFC1766	英語
DCTERMS.issued' scheme='DCTERMS.W3CDTF	2025-02-10
DC.identifier	https://doi.org/10.3847/1538-4357/ada364
DC.description	Takasao Shinsuke, Kunitomo Masanobu, Suzuki Takeru K., et al. Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm. The Astrophysical Journal 980, 111 (2025); https://doi.org/10.3847/1538-4357/ada364.
DCTERMS.abstract	Stellar spin is one of the fundamental quantities that characterize a star itself and its planetary system. Nevertheless, stellar spin-down mechanisms in protostellar and pre-main-sequence stellar phases have been a long-standing problem in star formation theory. To realize the spin-down, previous axisymmetric models based on the conventional magnetospheric paradigm have had to assume massive stellar winds or produce highly time-variable magnetospheric ejections. However, this picture has been challenged by both numerical simulations and observations. With a particular focus on the propeller regime for solar-mass stars, we propose a new picture of stellar spin-down based on our recent 3D magnetohydrodynamic simulation and stellar evolution calculation. We show that failed magnetospheric winds, unique to 3D models, significantly reduce the spin-up accretion torque, which make it easier for the star to spin-down. Additionally, the amplitude of time variability associated with magnetospheric ejections is reduced by 3D effects. Our simulation demonstrates that the star spins down by generating a conical disk wind, driven by a rotating stellar magnetosphere. Our theoretical estimates, inspired by the numerical model, suggest that the conical disk wind is likely to play a crucial role in extracting stellar angular momentum during the protostellar phase. As magnetospheric accretion is expected to occur in other accreting objects such as protogiant planets, this study will also contribute to the understanding of the angular momentum of such objects.
DC.rights	This article is licensed under a Creative Commons Attribution 4.0 International License.
DC.format	100435
citation_title	Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm
citation_author	Takasao, Shinsuke
	Kunitomo, Masanobu
	Suzuki, K. Takeru
	Iwasaki, Kazunari
	Tomida, Kengo
citation_publisher	American Astronomical Society
citation_language	英語
citation_date	2025-02-10
citation_journal_title	The Astrophysical Journal
citation_volume	980
citation_issue	1
citation_firstpage	111
citation_doi	https://doi.org/10.3847/1538-4357/ada364
citation_public_url	https://hdl.handle.net/11094/100435

Spin-down of Solar-mass Protostars in Magnetospheric Accretion Paradigm

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