论文标题
超新星反馈在附近星系星系中维持燃气湍流的证据
Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies
论文作者
论文摘要
HI和CO观察表明，星系中的冷气非常动荡。但是，预计湍流能量会迅速消散，这意味着需要一些能源来解释观察结果。这种湍流的性质尚不清楚，因为即使是主要候选人超新星（SN）的反馈也似乎不足。已经提出了其他机制，但没有达成一般共识。我们工作的主要新颖性是考虑到气盘的厚度和耀斑增加了湍流的耗散时间，从而降低了维持它所需的能量注入速率。与理论期望非常吻合，我们发现维持冷燃气湍流所需的SN能量的比例（又称SN偶联效率）为$ \ sim 1 $％，解决了长期存在的难题。
HI and CO observations indicate that the cold gas in galaxies is very turbulent. However, the turbulent energy is expected to be quickly dissipated, implying that some energy source is needed to explain the observations. The nature of such turbulence was long unclear, as even the main candidate, supernova (SN) feedback, seemed insufficient. Other mechanisms have been proposed, but without reaching a general consensus. The key novelty of our work is considering that the gas disc thickness and flaring increase the dissipation timescale of turbulence, thus reducing the energy injection rate required to sustain it. In excellent agreement with the theoretical expectations, we found that the fraction of the SN energy (a.k.a. SN coupling efficiency) needed to maintain the cold gas turbulence is $\sim 1$%, solving a long-standing conundrum.
