论文标题
在星系簇中大规模螺旋流的对流
Advection by large-scale spiral flows in galaxy clusters
论文作者
论文摘要
星系簇的簇内介质通常显示出延伸的准螺旋结构，该结构被称为冷锋（CFS）的切向不连续性强调。人们认为这些不连续性可以在内部（即下方）之间分离出低透镜，高金属气体（即下方），该CF从集群中心通过一些径向因子$ f_i $和高质量，高层，低金属气体在CF之外的CF之外，而CF被因子$ f_O $ $ f_O $推出。我们通过将熵和金属性不连续性与相应的方差平均值进行比较，使用新近depRection的热量剖面中的A2029，A2142，A2204，A2204和Centairus在文献中补充了CFS中补充了新的depRection热谱，从而发现了对这种图片的广泛支持。特别是，从熵和金属性分别推断出的平均对流因子$ f_k $和$ f_z $，强烈相关（$ \ Mathcal {r} = 0.7^{+0.2} _ { - 0.3} $）彼此之间，与较大的规模相关。 However, unlike sloshing simulations, in which the inside/outside phases are an inflow/outflow settling back to equilibrium after a violent perturbation, our results are more consistent with an outflow/inflow, with the fast, Mach $\mathcal{M}_i\sim0.8$ gas inside the CF being a rapidly heated or mixed outflow, probably originating from the cD galaxy, and gas outside the CF being a $ \ MATHCAL {M} _O \ SIM0.03 $，缓慢冷却的流入。特别是，熵表示外部对流因子$ f_ {ko} \ simeq 1.33 \ pm0.04 $，在所有CFS中大约是恒定的，在冷却时间内衡量了通过流动气体横穿的距离。相比之下，$ 1.1 \ Lessim f_ {ki} \ Lessim 2.5 $和$ 1 \ Lessim f_z \ sims 17 $ 17 $ 17 $在群集中差异很大，并且与病毒质量，$ f_ {ki {ki {ki {ki {ki {ki {ki} m_ {200}^{0.14 \ pm0.07} $和$ f_z \ propto m_ {200}^{1.4 \ pm0.4} $，这表明每个群集都具有准稳态的螺旋流。
The intracluster medium of a galaxy cluster often shows an extended quasi-spiral structure, accentuated by tangential discontinuities known as cold fronts (CFs). These discontinuities are thought to isolate between low-entropy, high-metallicity gas inside (i.e., below) the CF that was lifted from the center of the cluster by some radial factor $f_i$, and high-entropy, low-metallicity gas outside the CF that was pushed inward by a factor $f_o$. We find broad support for such a picture, by comparing the entropy and metallicity discontinuities with the respective azimuthal averages, using newly deprojected thermal profiles in clusters A2029, A2142, A2204 and Centaurus, supplemented by deprojected CFs from the literature. In particular, the mean advection factors $f_K$ and $f_Z$, inferred respectively from entropy and metallicity, strongly correlate ($\mathcal{R}=0.7^{+0.2}_{-0.3}$) with each other, consistent with large-scale advection. However, unlike sloshing simulations, in which the inside/outside phases are an inflow/outflow settling back to equilibrium after a violent perturbation, our results are more consistent with an outflow/inflow, with the fast, Mach $\mathcal{M}_i\sim0.8$ gas inside the CF being a rapidly heated or mixed outflow, probably originating from the cD galaxy, and gas outside the CF being a $\mathcal{M}_o\sim0.03$, slowly-cooling inflow. In particular, entropy indicates an outside advection factor $f_{Ko}\simeq 1.33\pm0.04$ that is approximately constant in all CFs, gauging the distance traversed by inflowing gas within a cooling time. In contrast, $1.1\lesssim f_{Ki}\lesssim 2.5$ and $1\lesssim f_Z\lesssim 17$ vary considerably among clusters, and strongly correlate ($3.1σ\text{-}4.2σ$) with the virial mass, $f_{Ki}\propto M_{200}^{0.14\pm0.07}$ and $f_Z\propto M_{200}^{1.4\pm0.4}$, suggesting that each cluster sustains a quasi-steady spiral flow.
