尘粒和原行星盘的共同演化。II.原行星盘的结构和演变:分析方法

IF 2.2 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Yusuke Tsukamoto
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引用次数: 0

摘要

在我们之前的研究(Tsukamoto et al. 2023b, PASJ, 75, 835)中,我们利用考虑了尘埃生长的三维非理想磁流体力学模拟研究了原行星盘的形成和早期演化,发现考虑了磁制动、尘埃生长和环极扩散的传统稳定吸积盘模型的修正方程很好地再现了模拟得到的盘结构(如密度和垂直磁场)。在本文中,作为之前研究的续篇,我们使用修正的稳定吸积盘模型,结合包层吸积的分析模型,分析研究了与0/I类年轻恒星天体相对应的原行星盘的结构和演化。我们估计,在圆盘形成初期,圆盘半径为几个天文单位,在吸积阶段结束时,半径会增加到几百个天文单位。磁盘质量估计为 0.01 美元 (lesssim M_{\rm disk}\对于一个半径为几十个天文单位、质量增殖速率为 $\dot{M}_\{rm disk} 的磁盘来说,M_odot$为 0.1 (lesssim 0.1, M_\odot$\sim 10^{-6}\, M_\odot \, {\rm yr^{-1}}$。这些估计值似乎与最近的观测结果一致。我们还发现,在典型的磁盘电离率(ζ ≳ 10-19 s-1)和中等质量增殖率($\dot{M}_\rm disk}gtrsim 10^{-8} \, M_\odot \,\, {\rm yr^{-1}}$)条件下,由于低等离子体β和高效的环极扩散,磁盘中的磁定向不稳定性被抑制了。我们认为,如果圆盘是通过磁制动演化的,那么圆盘外缘的比角动量(或旋转速度)径向剖面应该与包络面的比角动量(或旋转速度)径向剖面连续相连;如果圆盘是通过内部角动量传输过程(如引力不稳定性或磁动不稳定性)演化的,那么圆盘外缘的比角动量(或旋转速度)径向剖面应该是不连续的。未来对圆盘外缘的具体角动量分布进行详细观测,对于了解原行星盘的角动量传输机制非常重要。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Co-evolution of dust grains and protoplanetary disks. II. Structure and evolution of protoplanetary disks: An analytical approach
In our previous study (Tsukamoto et al. 2023b, PASJ, 75, 835), we investigated the formation and early evolution of protoplanetary disks with 3D non-ideal magnetohydrodynamics simulations considering dust growth, and found that the modified equations of the conventional steady accretion disk model that consider magnetic braking, dust growth, and ambipolar diffusion reproduce the disk structure (such as density and vertical magnetic field) obtained from simulations very well. In this paper, as a sequel to our previous study, we analytically investigate the structure and evolution of protoplanetary disks corresponding to Class 0/I young stellar objects using the modified steady accretion disk model combining an analytical model of envelope accretion. We estimate that the disk radius is several astronomical units at the disk formation epoch and increases to several hundred astronomical units at the end of the accretion phase. The disk mass is estimated to be $0.01 \lesssim M_{\rm disk} \lesssim 0.1 \, M_\odot$ for a disk with a radius of several tens of astronomical units and a mass accretion rate of $\dot{M}_{\rm disk} \sim 10^{-6} \, M_\odot \,\, {\rm yr^{-1}}$. These estimates seems to be consistent with recent observations. We also found that, with typical disk ionization rates (ζ ≳ 10−19 s−1) and a moderate mass accretion rate ($\dot{M}_{\rm disk}\gtrsim 10^{-8} \, M_\odot \,\, {\rm yr^{-1}}$), magnetorotational instability is suppressed in the disk because of low plasma β and efficient ambipolar diffusion. We argue that the radial profile of specific angular momentum (or rotational velocity) at the disk outer edge should be continuously connected to that of the envelope if the disk evolves by magnetic braking, and should be discontinuous if the disk evolves by an internal angular momentum transport process such as gravitational instability or magnetorotational instability. Future detailed observations of the specific angular momentum profile around the disk outer edge are important for understanding the angular momentum transport mechanism of protoplanetary disks.
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来源期刊
Publications of the Astronomical Society of Japan
Publications of the Astronomical Society of Japan 地学天文-天文与天体物理
CiteScore
4.10
自引率
13.00%
发文量
98
审稿时长
4-8 weeks
期刊介绍: Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.
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