Mecanism of Outflow form Dynamically Contracting Molecular Cores
Mecanism of Outflow form Dynamically Contracting Molecular Cores
批准号:
11640231
负责人:
TOMISAKA Kohji
金额:
$2.11万
依托单位国家:
日本
项目类别:
Grant-in-Aid for Scientific Research (C)
财政年份:
1999
资助国家:
日本
项目状态:
已结题
起止时间:
1999 至 2001
中文摘要
研究了星际分子云的动力学收缩。1. Tomisaka用嵌套网格轴对称磁流体力学模拟研究了分子外流的机理。分子云核心的旋转放大了环面磁场,使气体以分子外流的形式喷射出去。通过模拟,我们发现:(1)初始旋转速度指定了分子流出开始的时间。即增加角动量,在绝热核形成后立即发射出流。(2)当初始极向磁场较强(其能量与热磁场相当)时,形成U型流出,其中气体主要从距离旋转轴有限距离的一个形状为大写字母U的区域流出。(3)另一种是湍流流出,其中磁力线和速度场似乎是随机定向的,这是在初始磁能远小于热能的情况下实现的。在这种情况下,气体从整体上几乎垂直地从圆盘流出,流出物看起来像一个大写字母i。考虑到磁扩散,Nakamura研究了由强磁场支持的云的引力坍缩。(1)大质量模型在早期会导致大量高密度岩心破碎。这对应于星团形成模式。(2)相反,在质量较小的云中,条状物会生长,条状物会破碎成碎片。在这种情况下,将出现一个二进制系统。
英文摘要
Dynamical contraction of interstellar molecular clouds is studied. 1. Tomisaka studied the mechanism of molecular outflow with the nested-grid axi-symmetric magnetohydrodynamical simulations. Rotations of the molecular cloud cores amplify the toroidal magnetic fields, which eject the gas as molecular outflows. From the simulations, we explored the followings : (1) Initial rotation speed specifies the epoch when the molecular outflow begins. That is, increasing the angular momentum, the outflow is launched immediate after the adiabatic core is formed. (2) When the initial poloidal magnetic field is strong (its energy is comparable to the thermal one), a U-shaped outflow is formed, in which gas is mainly outflowing through a region whose shape looks like a capital letter U at a finite distance from the rotation axis. (3) The other is a turbulent outflow in which magnetic field lines and velocity fields seem to be randomly oriented, which is realized when the initial magnetic energy is much smaller than the thermal one. In this case, globally the gas moves out almost perpendicularly from the disk and the outflow looks like a capital letter I. 2. Nakamura studied the gravitational collapse of a cloud supported by strong magnetic fields taking into account of the magnetic diffusion. (1) A model with large mass leads to fragmentation to a number of high-densitycores in the early phase. This corresponds to a cluster forming mode. (2) Incontrast, in a less massive cloud a bar grows and the bar breaks into fragments. In this case a binary system will appear.
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F.Nakamura, Zhi-Yun Li: "Nonaxisymmetric Evolution of Magnetically Subcritical Clouds : Bar Growth, Core Elongation, and Binary Formation"The Astrophysical Journal. 566. L101-L104 (2002)
F.Nakamura、Zhi-Yun Li:“磁亚临界云的非轴对称演化:棒生长、核心伸长和双星形成”天体物理学杂志。
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K.Tomisaka: "Collapse-Driven Outflow in Star-Forming Molecular Cores"in "Star Formation 1999". 197-198 (2000)
K.Tomisaka:《恒星形成 1999》中的“恒星形成分子核心中的塌缩驱动流出”。
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F. Nakamura: "Formation of an Mailing Diskiike Envelope around a Protostar"The Astrophysical Journal. 543. 291-298 (2000)
F. Nakamura:“围绕原恒星形成邮寄 Diskiike 信封”《天体物理学杂志》。
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K.Tomisaka: "Outflow from YSO and Angular Momentum Transfer"in Proceedings of the IAU Simposium on "The Formation of Binary Stars". 401-405 (2001)
K.Tomisaka:“YSO 的流出和角动量转移”,IAU 研讨会“双星形成”会议记录。
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F.Nakamura: "Formation of an Infalling Disklike Envelope around a Protostar"The Astrophysical Journal. 543. 291-298 (2000)
F.Nakamura:“围绕原恒星形成内落盘状包络”《天体物理学杂志》。
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