论文标题
预期的fu ori爆发幅度从光学到中红外
Expected FU Ori Outburst Amplitudes from the Optical to the Mid-Infrared
论文作者
论文摘要
在年轻恒星物体周围（YSO）周围的磁盘由材料组成，这些材料由中心恒星的被动加热以及由于质量积聚而产生的活性，粘性加热提供的能量。 Fu Ori恒星是YSO，其内部磁盘区域的积聚率大大提高。作为磁盘从标准低状态到fu ori样高状态积聚的过渡，爆发通过光度亮度在广泛的波长上表现出来。我们提出了预期的亮度幅度$ \ sim $4000Å和8 $μ$ m的预期振幅 - 最常见的Fu Ori类型爆发事件的波长范围。我们的模型由一个具有低积聚状态的光学厚的被动$+$ Active稳态积聚磁盘。
Disks around young stellar objects (YSOs) consist of material that thermally emits the energy provided by a combination of passive heating from the central star, and active, viscous heating due to mass accretion. FU Ori stars are YSOs with substantially enhanced accretion rates in their inner disk regions. As a disk transitions from standard low-state, to FU Ori-like high-state accretion, the outburst manifests through photometric brightening over a broad range of wavelengths. We present results for the expected amplitudes of the brightening between $\sim$4000 Å and 8 $μ$m -- the wavelength range where FU Ori type outburst events are most commonly detected. Our model consists of an optically thick passive $+$ active steady-state accretion disk with low and high accretion states.
