Turbulence has the potential for creating gas density enhancements that initiate cloud and star formation (SF), and it can be generated locally by SF. To study the connection between turbulence and SF, we looked for relationships between SF traced by FUV images, and gas turbulence traced by kinetic energy density (KED) and velocity dispersion (v _disp) in the LITTLE THINGS sample of nearby dIrr galaxies. We performed 2D cross-correlations between FUV and KED images, measured cross-correlations in annuli to produce correlation coefficients as a function of radius, and determined the cumulative distribution function of the cross-correlation value. We also plotted on a pixel-by-pixel basis the locally excess KED, v _disp, and H i mass surface density, Σ_HI, as determined from the respective values with the radial profiles subtracted, versus the excess SF rate density Σ_SFR, for all regions with positive excess Σ_SFR. We found that Σ_SFR and KED are poorly correlated. The excess KED associated with SF implies a ∼0.5% efficiency for supernova energy to pump local H i turbulence on the scale of the resolution here, which is a factor of ∼2 too small for all of the turbulence on a galactic scale. The excess v _disp in SF regions is also small, only ∼0.37 km s⁻¹. The local excess in Σ_HI corresponding to an excess in Σ_SFR is consistent with a H i consumption time of ∼1.6 Gyr in the inner parts of the galaxies. The similarity between this timescale and the consumption time for CO implies that CO-dark molecular gas has comparable mass to H i in the inner disks.

湍流具有产生气体密度增强的潜力，从而引发云和恒星形成 (SF)，并且可以由 SF 局部产生。为了研究湍流和 SF 之间的联系，我们在附近 dIrr 星系的 LITTLE THINGS 样本中寻找了由 FUV 图像追踪的 SF 与由动能密度 (KED) 和速度色散 ( v _disp )追踪的气体湍流之间的关系。我们在 FUV 和 KED 图像之间进行了 2D 互相关，测量环中的互相关以产生作为半径函数的相关系数，并确定互相关值的累积分布函数。我们还逐个像素地绘制了局部过量的 KED、v _disp和 H i质量表面密度，Σ _HI，如从相应的值来确定与减去径向分布，相对于过量SF率密度Σ _SFR，对于具有正的过量Σ所有区域_的SFR。我们发现 Σ _SFR和 KED 的相关性很差。与 SF 相关的过量 KED 意味着超新星能量在此处分辨率尺度上泵送局部 H i湍流的效率约为 0.5%，对于银河尺度上的所有湍流来说，这个系数太小了 2 倍。SF 区域中的过量v _disp也很小，只有 ~0.37 km s ^-1。Σ _HI的局部超额对应于 Σ _SFR的超额与星系内部约 1.6 Gyr的 H i消耗时间一致。这个时间尺度与 CO 消耗时间之间的相似性意味着 CO 暗分子气体的质量与内部圆盘中的H i相当。