论文标题
Gaia 18dvy：Cygnus OB3协会的新福尔
Gaia 18dvy: a new FUor in the Cygnus OB3 association
论文作者
论文摘要
我们以1.88 kpc的距离呈现位于Cygnus OB3关联中的GAIA18DVY的光学光度和光谱观测。当盖亚警报系统的Lightcurve在2018 - 2019年显示$ \ gtrsim $ 4 MAG上升时，该物体是由Gaia Alerts系统注明的。在中型波长下还可以观察到亮度。随着爆发的发展，Gaia18dvy的红外颜色变得更蓝。它在爆发阶段的光学和近红外光谱特性与真正的fu fuder fu orionis型年轻喷发恒星一致。爆发的祖细胞可能是一个低质量的K型星，光学灭绝为$ \ sim $ 3 mag。基于静态光谱能量分布的间隔结构的辐射传输建模表示磁盘的质量为$ 4 {\ times} 10^{ - 3} \，m _ {\ odot} $。我们的简单积聚磁盘建模意味着，直到2019年中期，增生率已成倍增加了3年以上，当时它达到了$ 6.9 \ times 10^{ - 6} \，m _ {\ odot} $ yr $ yr $^{ - 1} $。在许多方面，gaia18dvy类似于fu ori-type对象HBC 722
We present optical-infrared photometric and spectroscopic observations of Gaia18dvy, located in the Cygnus OB3 association at a distance of 1.88 kpc. The object was noted by the Gaia alerts system when its lightcurve exhibited a $\gtrsim$4 mag rise in 2018-2019. The brightening was also observable at mid-infared wavelengths. The infrared colors of Gaia18dvy became bluer as the outburst progressed. Its optical and near-infrared spectroscopic characteristics in the outburst phase are consistent with those of bona fide FU Orionis-type young eruptive stars. The progenitor of the outburst is probably a low-mass K-type star with an optical extinction of $\sim$3 mag. A radiative transfer modeling of the circumstellar structure, based on the quiescent spectral energy distribution, indicates a disk with a mass of $4{\times}10^{-3}\,M_{\odot}$. Our simple accretion disk modeling implies that the accretion rate had been exponentially increasing for more than 3 years until mid-2019, when it reached a peak value of $6.9 \times 10^{-6}\,M_{\odot}$yr$^{-1}$. In many respects, Gaia18dvy is similar to the FU Ori-type object HBC 722
