发现来自单个HAe/Be星HD 100546的喷流
Discovery of a jet from the single HAe/Be star HD 100546
摘要：
年轻的吸积恒星驱动外流，准直成喷流，这可以看到数百au从他们的驱动源。吸积和外流活动随着系统年龄的增长而停止，据信磁离心发射的盘风是调节通过原行星盘吸积的关键因素。在经典T~Tauri星（$M_\star\lesssim2\,M_\odot$）中，原恒星喷流已被研究得很好，而在附近的中等质量恒星（$d\lesssim150\,$）中，也就是赫比格Ae/Be星，却很少有喷流被探测到。本文报道了Herbig~Ae/Be星HD~100546的VLT/MUSE观测和原恒星喷流的发现。喷流在外观上类似于低质量恒星驱动的喷流，并与HD~163296的喷流进行了很好的比较，HD ~163296是附近Herbig~Ae/Be恒星的唯一其他已知光学喷流。我们推导出$\log \dot{M}_{jet} \sim -9.5$喷流的（单侧）质量损失率（在$M_\odot$ \，yr $^{-1}$中）和流出物与吸积物的比率大约为$3\times10^{-3}$，低于CTTS喷流的比率。HD~100546喷流的发现特别有趣，因为HD~100546周围的原行星盘显示出一个大的径向间隙，螺旋结构，可能存在一个原行星系统。以前在H $α$和VLT/SPHERE中看到的一个棒状结构与喷流位置角相同，可能代表喷流的底部，并表明在约2.au范围内有一个喷流发射区。我们的结论是，在半径超过几个AU的磁盘的演变不影响系统的能力，发射喷气机。
英文摘要：
Young accreting stars drive outflows that collimate into jets, which can be seen hundreds of au from their driving sources. Accretion and outflow activity cease with system age, and it is believed that magneto-centrifugally launched disk winds are critical agents in regulating accretion through the protoplanetary disk. Protostellar jets are well studied in classical T~Tauri stars ($M_\star\lesssim2\,M_\odot$), while few nearby ($d\lesssim150\,$pc) intermediate-mass stars ($M_\star=2-10\,M_\odot$), known as Herbig Ae/Be stars, have detected jets. We report VLT/MUSE observations of the Herbig~Ae/Be star HD~100546 and the discovery of a protostellar jet. The jet is similar in appearance to jets driven by low-mass stars and compares well with the jet of HD~163296, the only other known optical jet from a nearby Herbig~Ae/Be star. We derive a (one-sided) mass-loss rate in the jet of $\log \dot{M}_{jet} \sim -9.5$ (in $M_\odot$\,yr$^{-1}$) and a ratio of outflow to accretion of roughly $3\times10^{-3}$, which is lower than that of CTTS jets. The discovery of the HD~100546 jet is particularly interesting because the protoplanetary disk around HD~100546 shows a large radial gap, spiral structure, and might host a protoplanetary system. A bar-like structure previously seen in H$α$ with VLT/SPHERE shares the jet position angle, likely represents the base of the jet, and suggests a jet-launching region within about 2\,au. We conclude that the evolution of the disk at radii beyond a few au does not affect the ability of the system to launch jets.
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