论文标题
核星爆圈的银河风和气泡
Galactic winds and bubbles from nuclear starburst rings
论文作者
论文摘要
来自本地Starburst星系的银河流出通常表现出分层的几何形状，$ 10^4 \，$ K流垫圈更热$ 10^7 \，$ K，$ K，圆柱体聚集，X射线发射等离子体。在这里，我们认为在环形几何形状中通过能量注射驱动的风可以产生这种独特的大规模多相形态。环构型的动机是通过观察到的，即大量的年轻恒星簇通常分布在主机Galaxy的内林布拉德共鸣的环中，那里大规模的螺旋臂结构终止。我们提出了参数化的三维辐射流体动力学模拟，遵循Starburst环的能量驱动的热风的出现和动力学。 In this Letter, we show that the flow shocks on itself within the inner ring hole, maintaining high $10^7$\,K temperatures, whilst flows that emerge from the wind-driving ring unobstructed can undergo rapid bulk cooling down to $10^4\,$K, producing a fast hot bi-conical outflow enclosed by a sheath of cooler nearly co-moving material without ram-pressure acceleration.即使在没有银河磁盘或磁场的压力约束的情况下，热流也沿着环轴准直。在扩张的早期阶段，新兴风形成了类似气泡的形状，让人联想到银河系的色素和费米气泡，并且可以达到通常与AGN驱动风相关的速度。我们讨论了环构型的物理，辐射散装冷却的条件以及对未来X射线观测的影响。
Galactic outflows from local starburst galaxies typically exhibit a layered geometry, with cool $10^4\,$K flow sheathing a hotter $10^7\,$K, cylindrically-collimated, X-ray emitting plasma. Here, we argue that winds driven by energy-injection in a ring-like geometry can produce this distinctive large-scale multi-phase morphology. The ring configuration is motivated by the observation that massive young star clusters are often distributed in a ring at the host galaxy's inner Lindblad resonance, where larger-scale spiral arm structure terminates. We present parameterized three-dimensional radiative hydrodynamical simulations that follow the emergence and dynamics of energy-driven hot winds from starburst rings. In this Letter, we show that the flow shocks on itself within the inner ring hole, maintaining high $10^7$\,K temperatures, whilst flows that emerge from the wind-driving ring unobstructed can undergo rapid bulk cooling down to $10^4\,$K, producing a fast hot bi-conical outflow enclosed by a sheath of cooler nearly co-moving material without ram-pressure acceleration. The hot flow is collimated along the ring axis, even in the absence of pressure confinement from a galactic disk or magnetic fields. In the early stages of expansion, the emerging wind forms a bubble-like shape reminiscent of the Milky Way's eROSITA and Fermi bubbles and can reach velocities usually associated with AGN-driven winds. We discuss the physics of the ring configuration, the conditions for radiative bulk cooling, and the implications for future X-ray observations.
