论文标题
使用碎屑盘观测来推断父行星内或外部绕或外部旋转的近地伴侣
Using debris disk observations to infer substellar companions orbiting within or outside a parent planetesimal belt
论文作者
论文摘要
目标。我们分析了源自替代伴侣的世俗扰动对碎屑磁盘中的灰尘动力学的影响是否可以通过空间分辨的观察结果进行研究。 方法。我们在数值上模拟了光谱A3V型星星周围狭窄和怪异的冷行星的碰撞演变，该皮带被旋转的伴侣与恒星更接近或更远的恒星旋转。根据由此产生的空间灰尘分布，我们在$ k $，$ n $和$ q $ bands中模拟了其表面亮度的空间解析图，并以70美元$ $ m和1300 $ $ $ m的波长为70 $ $ $ m。 结果。假设看到附近的碎屑盘面对面，我们发现亮度分布随观测波长而变化很大，例如在$ n $和$ q $ band之间。这可以通过在井喷极限附近的最小晶粒发射的相对贡献来解释。由于皮带向内绕着旋转的伴侣诱导的世俗扰动，形成光环和靠近母体皮带的大晶粒的小晶粒的轨道。光环由较旧的谷物组成，沿着皮带沿着。尾随的幅度随着垂直质量的增加而降低，因此随着扰动强度的增加而降低，这是我们通过将椭圆形成恒定亮度的线条，在表面亮度的合成图中恢复的趋势。具有外部垂直的系统不会显示出均匀的光环动力，因为小晶粒的轨道发生了强烈改变。我们确定了亮度分布的特征，适合于区分具有可能可检测到的内部或外部透视器的系统，尤其是在$ q $频段中与JWST/MIRI的合并观察结果，以追踪小谷物发射，并在MM波长处以追溯父行星的位置的MM波长。
Aims. We analyze whether the effects of secular perturbations, originating from a substellar companion, on the dust dynamics in a debris disk can be investigated with spatially resolved observations. Methods. We numerically simulated the collisional evolution of narrow and eccentric cold planetesimal belts around a star of spectral type A3V that are secularly perturbed by a companion that orbits either closer to or farther from the star than the belt. Based on the resulting spatial dust distributions, we simulated spatially resolved maps of their surface brightness in the $K$, $N$, and $Q$ bands and at wavelengths of 70$μ$m and 1300$μ$m. Results. Assuming a nearby debris disk seen face-on, we find that the brightness distribution varies significantly with observing wavelength, for example between the $N$ and $Q$ band. This can be explained by the varying relative contribution of the emission of the smallest grains near the blowout limit. The orbits of both the small grains that form the halo and the large grains close to the parent belt precess due to the secular perturbations induced by a companion orbiting inward of the belt. The halo, being composed of older grains, trails the belt. The magnitude of the trailing decreases with increasing perturber mass and hence with increasing strength of the perturbation, a trend we recovered in synthetic maps of surface brightness by fitting ellipses to lines of constant brightness. Systems with an outer perturber do not show a uniform halo precession since the orbits of small grains are strongly altered. We identified features of the brightness distributions suitable for distinguishing between systems with a potentially detectable inner or outer perturber, especially with a combined observation with JWST/MIRI in the $Q$ band tracing small grain emission and with ALMA at mm wavelengths tracing the position of the parent planetesimal belt.
