论文标题
Edge-On的可见和近红外的光谱间距分析是Star $ beaquarii
Visible and near-infrared spectro-interferometric analysis of the edge-on Be star $ο$ Aquarii
论文作者
论文摘要
我们提供了来自Quasi-Contemocanous Chara/Vega和Vlti/Amber观测值的Be-Shell Star $ aquarii的详细可见且近红外的触觉分析分析。我们测量了$ o aquarii的恒星半径为4.0 $ \ pm $ 0.3 $ \ mathrm {r _ {\ odot}} $。我们使用运动学模型和MCMC拟合程序限制了磁盘几何形状和运动学。 h $α$和br $γ$中的磁盘尺寸相似，$ \ sim $ 10-12 $ \ mathrm {d _ {\ star}} $，这并不常见，因为大多数结果是明星的大多数结果显示出H $α$比BR $γ$更大的延伸。我们发现，源自H $α$的倾斜角$ i $明显低（$ \ sim $ 15摄入），比br $γ$衍生的倾斜度$ $ $。发现磁盘运动学接近Br $γ$的开普勒旋转，但在h $α$中却不接近。在使用HDUST模型网格（Beatlas）分析我们的所有数据之后，我们在两行中找到了磁盘的常见物理描述：$σ_{0} $ = 0.12 g cm \ textsuperscript {-2}和$ m $ = 3.0。发现恒星旋转速率与临界值非常接近（$ \ sim $ 96 \％）。我们对多个上述h $α$轮廓和成像极化法的分析表明，该磁盘至少稳定了20年。与Br $γ$相比，H $α$中的数据显示出实质上不同的图片，使用当前的BE Star Disk的物理模型无法完全理解。 $ o aquarii显示了一个稳定的磁盘，但测得的$ m $低于稳态VDD模型中的标准值。可以从该恒星的高旋转速率来理解这种长期稳定性，该速率是磁盘中质量注入的主要来源。我们在恒星旋转和磁盘稳定性方面的结果与文献中的结果一致，表明晚期恒星更可能是快速旋转器并且具有稳定的磁盘。
We present a detailed visible and near-IR spectro-interferometric analysis of the Be-shell star $ο$ Aquarii from quasi-contemporaneous CHARA/VEGA and VLTI/AMBER observations. We measured the stellar radius of $ο$ Aquarii as 4.0 $\pm$ 0.3 $\mathrm{R_{\odot}}$. We constrained the disk geometry and kinematics using a kinematic model and a MCMC fitting procedure. The disk sizes in H$α$ and Br$γ$ were found to be similar, at $\sim$10-12 $\mathrm{D_{\star}}$, which is uncommon since most results for Be stars show a larger extension in H$α$ than in Br$γ$. We found that the inclination angle $i$ derived from H$α$ is significantly lower ($\sim$15 deg) than the one derived from Br$γ$. The disk kinematics were found to be near to the Keplerian rotation in Br$γ$, but not in H$α$. After analyzing all our data using a grid of HDUST models (BeAtlas), we found a common physical description for the disk in both lines: $Σ_{0}$ = 0.12 g cm\textsuperscript{-2} and $m$ = 3.0. The stellar rotational rate was found to be very close ($\sim$96\%) to the critical value. Our analysis of multi-epoch H$α$ profiles and imaging polarimetry indicates that the disk has been stable for at least 20 years. Compared to Br$γ$, the data in H$α$ shows a substantially different picture that cannot fully be understood using the current physical models of Be star disks. $ο$ Aquarii presents a stable disk, but the measured $m$ is lower than the standard value in the VDD model for steady-state. Such long-term stability can be understood in terms of the high rotational rate for this star, the rate being a main source for the mass injection in the disk. Our results on the stellar rotation and disk stability are consistent with results in the literature showing that late-type Be stars are more likely to be fast rotators and have stable disks.
