论文标题
Fuor型年轻爆发星V346 Normae中的信封到磁盘质量运输
Envelope-to-disk mass transport in the FUor-type young eruptive star V346 Normae
论文作者
论文摘要
在10 $^{ - 4} \，m _ {\ odot} $/yr的顺序上具有磁盘到明星的积聚率，fu orionis-type stars（fuors）被认为是情节增生的可见示例。燃料通常被大规模的信封包围，这些信封可以补充磁盘材料，并使磁盘能够产生积聚爆发。我们观察到Fuor-type Star V346或Alma在1.3 mm连续体和不同的CO旋转线上观察到。我们绘制了其包膜的密度和速度结构，并使用通道图，位置 - 速度图和光谱式估计方法分析了结果。我们在0.1 $ m _ {\ odot} $中心星周围发现了一个伪盘和一个开普勒磁盘。我们确定了从信封上的输入速率到6 $ \ times $ 10 $^{ - 6} \，m _ {\ odot} $/yr的磁盘，比从磁盘上的静态积聚率高的百分比高。这暗示了插入率和增生率之间的不匹配是爆发的原因。
Having disk-to-star accretion rates on the order of 10$^{-4}\,M_{\odot}$/yr, FU Orionis-type stars (FUors) are thought to be the visible examples for episodic accretion. FUors are often surrounded by massive envelopes, which replenish the disk material and enable the disk to produce accretion outbursts. We observed the FUor-type star V346 Nor with ALMA at 1.3~mm continuum and in different CO rotational lines. We mapped the density and velocity structure of its envelope and analyzed the results using channel maps, position-velocity diagrams, and spectro-astrometric methods. We discovered a pseudo-disk and a Keplerian disk around a 0.1 $M_{\odot}$ central star. We determined an infall rate from the envelope onto the disk of 6$\times$10$^{-6}\,M_{\odot}$/yr, a factor of few higher than the quiescent accretion rate from the disk onto the star. This hints for a mismatch between the infall and accretion rates as the cause of the eruption.
