论文标题
大规模二元系统HD的风碰撞和积聚模拟166734
Wind Collision and Accretion Simulations of the Massive Binary System HD 166734
论文作者
论文摘要
我们运行流体动力模拟，沿其二进制轨道沿巨大的二元系统HD 166734的碰撞风结构，并表明接近Periastron通道接近二次风被抑制，次生会产生。该系统组成了两个蓝色超级巨人，质量为$ M_1 \约39.5〜 \ rm {m_ \ odot} $和$ m_2 \ of 30.5〜〜 \ rm {m_ \ odot} $，在$ p \ simeq 34.538〜 \ rm {days days} $ eccentricity上，$ p \ simeq 34.538〜 \ rm通过X射线中的轨道观察到这种具有较高偏心率的O-O二元二进制，在那里它显示出不寻常的长度最小值接近Periastron通道。我们使用高级模拟，并以风加速和处方处理积聚，并以高分辨率模拟整个轨道，以捕获风中的不稳定性。我们发现，即使在Apastron，碰撞的风结构也不稳定。随着恒星接近periastron通道，二次风被主风淬灭，并开始吸收次级。积聚阶段持续$ \ simeq 12〜 \ rm {days} $，我们获得的每个周期的积聚质量量为$ m _ {\ rm {acc}} \ simeq 1.3 \ cdot 10^{ - 8}〜\ rm {m_ \ odot} $。积聚阶段可以解释系统从系统中观察到的X射线发射下降。
We run hydrodynamic simulations which follow the colliding winds structure of the massive binary system HD 166734 along its binary orbit, and show that close to periastron passage the secondary wind is suppressed and the secondary accretes mass from the primary wind. The system consists two blue supergiants with masses of $M_1 \approx 39.5 ~\rm{M_\odot}$ and $M_2 \approx 30.5 ~\rm{M_\odot}$, on a $P \simeq 34.538 ~\rm{days}$ orbit with eccentricity of $e \approx 0.618$. This close O-O binary with high eccentricity is observed through its orbit in the X-rays, where it shows an unusual long minimum close to periastron passage. We use advanced simulations with wind acceleration and prescription treatment of accretion and simulate the entire orbit at high resolution that captures the instabilities in the winds. We find that the colliding wind structure is unstable even at apastron. As the stars approach periastron passage the secondary wind is quenched by the primary wind and the accretion onto the secondary begins. The accretion phase lasts for $\simeq 12 ~\rm{days}$, and the amount of accreted mass per cycle we obtain is $M_{\rm{acc}} \simeq 1.3 \cdot 10^{-8} ~\rm{M_\odot}$. The accretion phase can account for the observed decline in X-ray emission from the system.
