论文标题
混合簇内培养基和星系簇的通用熵轮廓的准螺旋溶液
Quasi-spiral solution to the mixed intracluster medium and the universal entropy profile of galaxy clusters
论文作者
论文摘要
排除良好的星系簇通常在depRotded密度$ρ$和温度$ t $ fields中显示出大型的准螺旋结构，并通过切向偏见的切线不连续性叠加在通用的radial熵配置文件上，并用线性$ k（r）\ propte t propto propto r $ rad propto r propto r $ radiage coldiage。我们表明，螺旋结构为混合簇内培养基（ICM）提供了天然的准平稳溶液，引入了限制局部浮力或重等离子体相的适度压力螺旋。该解决方案在存在均匀或差分旋转的情况下持续存在，并且可以容纳流入和流出。流体动力绝热模拟具有扰动，使角动量沉积并混合血浆，从而使渐近螺旋结构渐近。我们在2D和3D的Eulerian和Lagrangian模拟中发现了类似的螺旋，并合并和偏移，簇。 The discontinuity surface is given in spherical coordinates $\{r,θ,ϕ\}$ by $ϕ(r,θ)\propto Φ(r)$, where $Φ$ is the gravitational potential, combining a trailing spiral in the equatorial ($θ=π/2$) plane and semicircles perpendicular to the plane, in resemblance of a snail shell.当地的对流不稳定可以在螺旋式绕组之间发展，促进了Sublinear $ k（r）$区域的改进的全球不稳定；因此，即使在消散后，也会进化出的螺旋形印记在ICM上。螺旋结构带来了冷热相处的接近度，表明即使在存在辐射冷却的情况下，观察到的快速流出也可以维持结构。
Well-resolved galaxy clusters often show a large-scale quasi-spiral structure in deprojected density $ρ$ and temperature $T$ fields, delineated by a tangential discontinuity known as a cold front, superimposed on a universal radial entropy profile with a linear $K(r)\propto Tρ^{-2/3}\propto r$ adiabat. We show that a spiral structure provides a natural quasi-stationary solution for the mixed intracluster medium (ICM), introducing a modest pressure spiral that confines the locally buoyant or heavy plasma phases. The solution persists in the presence of uniform or differential rotation, and can accommodate both an inflow and an outflow. Hydrodynamic adiabatic simulations with perturbations that deposit angular momentum and mix the plasma thus asymptote to a self-similar spiral structure. We find similar spirals in Eulerian and Lagrangian simulations of 2D and 3D, merger and offset, clusters. The discontinuity surface is given in spherical coordinates $\{r,θ,ϕ\}$ by $ϕ(r,θ)\propto Φ(r)$, where $Φ$ is the gravitational potential, combining a trailing spiral in the equatorial ($θ=π/2$) plane and semicircles perpendicular to the plane, in resemblance of a snail shell. A local convective instability can develop between spiral windings, driving a modified global instability in sublinear $K(r)$ regions; evolved spirals thus imprint the observed $K\propto r$ onto the ICM even after they dissipate. The spiral structure brings hot and cold phases to close proximity, suggesting that the observed fast outflows could sustain the structure even in the presence of radiative cooling.
