Title: Asymmetric radiation in binary systems: Implications for disk evolution and chemistry Show Chinese title

Title: 双星系统中的不对称辐射：对盘演化和化学的影响

Abstract: Current models of binary systems often depend on simplified approach of the radiation field, which are unlikely to accurately capture the complexities of asymmetric environments. We investigate the dynamical and chemical implications of a 3D asymmetric radiation field that accounts for the optical properties of sub-structures present in a protoplanetary disk, as well as the inclusion of a secondary radiation source in binary systems. We conducted a series of 3D-SPH hydrodynamical simulations using PHANTOM, coupled with the 3D Monte Carlo radiative transfer code MCFOST, to compute disc temperatures on-the-fly. We explored different binary-disk orientations (0$^o$ and 30$^o$) for an eccentric binary, along with a constant dust-to-gas ratio and dust as a mixture prescription. We also simulated an outburst event as an example of a drastic increase in luminosity. Heating from the secondary star inflates the outer disk, increasing the aspect ratio facing the companion by about 25% in inclined cases compared to 10% in coplanar ones. Dust settling in the mid-plane enhances extinction along the disk plane, making the coplanar case cooler than the inclined one on the side of the disk facing the companion. Besides, heating causes a shift in the snow line for species with freeze-out temperatures below 50 K, depending on the disk-binary inclination and binary phase. During outbursts, the aspect ratio doubles on the star-facing side and increases by 50% on the opposite side in inclined cases. The snow line shift would impact all the species considered in the outburst case. Disk heating in binaries depends on stellar properties, orbital phase, and disk local and global characteristics. This results in temperature asymmetries, especially during secondary star outbursts, leading to variations in aspect ratio and snow lines that can affect chemistry and planet formation. Show Chinese abstract

Abstract: 当前双星系统的模型通常依赖于辐射场的简化方法，这些方法不太可能准确捕捉不对称环境的复杂性。 我们研究了考虑原行星盘中子结构的光学特性以及双星系统中第二个辐射源的3D不对称辐射场的动力学和化学影响。 我们使用PHANTOM进行了系列3D-SPH流体动力学模拟，并结合3D蒙特卡洛辐射转移代码MCFOST，在线计算了盘温度。 我们探索了偏心双星的不同双星-盘取向（0$^o$和30$^o$），同时保持恒定的尘埃-气体比和尘埃作为混合物的处理方式。 我们还模拟了一个爆发事件，作为光度急剧增加的例子。 来自次级恒星的加热膨胀了外盘，在倾斜情况下，相对于共面情况，面对伴星的剖面比增加了约25%。 中间平面的尘埃沉降增强了盘平面的消光，使得在面对伴星的盘的一侧，共面情况比倾斜情况更冷。 此外，加热会导致冻结温度低于50 K的物种的雪线发生位移，具体取决于盘-双星倾角和双星相位。 在爆发期间，倾斜情况下面向恒星的一侧的剖面比翻倍，而另一侧则增加了50%。 雪线的位移将影响爆发情况下所有考虑的物种。 双星中的盘加热取决于恒星特性、轨道相位以及盘的局部和全局特征。 这导致了温度不对称性，特别是在次级恒星爆发期间，导致剖面比和雪线的变化，这可能会影响化学过程和行星形成。