论文标题
二进制中的碎屑盘：形态和光度特征
Debris discs in binaries: morphology and photometric signatures
论文作者
论文摘要
我们的目的是查看伴侣的存在是否会影响两颗恒星之间的碎屑带，以及是否会留下任何可检测到的特征，这些特征可以通过当前或将来的仪器观察到。我们考虑了一个围护的母体（PB）行星，该皮带位于2颗星之间的稳定性限制内，并使用染色器代码遵循该PB带产生的粉尘的耦合动力学和碰撞演化。我们探索几个免费参数，例如皮带的质量或二进制的质量比和轨道。我们使用Grater封装来生成2-D光度图和系统集成的SED。我们证实了通过较早的Dycoss研究获得的初步结果，即碰撞活性，二元扰动和恒星辐射压力的耦合作用在2颗恒星之间动态不稳定区域中保持小晶粒的光环。此外，确定了几个空间结构，尤其是一个从PB带一直延伸到伴侣恒星的单个螺旋臂。我们还确定了二颗恒星周围的淡淡，更紧凑的光盘，该恒星是非本地恒星，并从不稳定的光环中脱离小晶粒。光环，螺旋臂和次级圆盘都应通过类似于球体的能力的仪器在分辨的图像上检测到。与无伴随的情况相比，整个系统在小晶粒中耗尽。这种耗竭在系统的集成SED上留下了烙印，它看起来比单星围绕同一家长的身体皮带更冷。这一新发现可以解释为什么某些未解决的二线碟片的SED衍生位置$ r_ {disc} $将其主要腰带置于2颗星之间的动态“禁止”区域：这种明显的悖论确实可能是由于使用$ r_ {disc} $有效的单一star casecriptions to him of the star case
We aim to see whether debris belts evolving in between two stars may be impacted by the presence of the companion and whether this leaves any detectable signature that could be observed with current or future instruments. We consider a circumprimary parent body (PB) planetesimal belt that is placed just inside the stability limit between the 2 stars and use the DyCoSS code to follow the coupled dynamical and collisional evolution of the dust produced by this PB belt. We explore several free parameters such as the belt's mass or the binary's mass ratio and orbit. We use the GraTeR package to produce 2-D luminosity maps and system-integrated SEDs. We confirm a preliminary result obtained by earlier DyCoSS studies, which is that the coupled effect of collisional activity, binary perturbations and stellar radiation pressure maintains a halo of small grains in the dynamically unstable region between the 2 stars. In addition, several spatial structures are identified, notably a single spiral arm stretching all the way from the PB belt to the companion star. We also identify a fainter and more compact disc around the secondary star, which is non-native and feeds off small grains from the unstable halo. Both the halo, spiral arm and secondary disc should be detectable on resolved images by instruments with capacities similar to SPHERE. The system as a whole is depleted in small grains when compared to a companion-free case. This depletion leaves an imprint on the system's integrated SED, which appears colder than for the same parent body belt around a single star. This new finding could explain why the SED-derived location $r_{disc}$ of some unresolved discs-in-binaries places their primary belt in the dynamically "forbidden" region between the 2 stars: this apparent paradox could indeed be due to overestimating $r_{disc}$ when using empirical prescriptions valid for a single star case
