论文标题
NGC 6334的多尺度物理特性，如磁场，密度梯度，速度梯度和重力之间的局部相对取向所揭示
Multi-scale physical properties of NGC 6334 as revealed by local relative orientations between magnetic fields, density gradients, velocity gradients, and gravity
论文作者
论文摘要
我们在巨大的恒星形成区域NGC 6334中提出了对4个团块（I（n），I，IV和V）的Alma尘埃极化和分子线观测。与JCMT，Planck和Nanten2之间的大规模灰尘极化和分子线数据相结合，我们使尘埃粉尘极化和分子线数据相结合，我们使我们之间的磁场分析是协同的磁力分析。 （$θ_ {\ MathRM {b}} $），列密度梯度（$θ_ {\ MathRM {ng}} $），局部重力（$θ_ {\ Mathrm {lg}} $），以及velocity梯度（$ tem MELLI） （从$ \ sim $ 30 PC到0.003 PC）NGC 6334中的物理属性。我们发现$θ_ {\ Mathrm {b}} $和$θ_ {\ Mathrm {ng Mathrm {ng}} $从统计上始终的始终变化到柱状平行的变化， （$ n _ {\ mathrm {h_2}} $）增加了，这是以前数值研究所揭示的复杂/云量表的tho to-sub-alfvénic湍流的签名。因为$θ_ {\ mathrm {ng}} $和$θ_ {\ Mathrm {lg}} $优先在NGC 6334云中对齐，我们建议$θ_{\ Mathrm {b} $ the $ the $ the $ the $ the \ the \ ngrm { $ n _ {\ mathrm {h_2}} $是因为磁场线被重力拖动。在更高的$ n _ {\ mathrm {h_2}} $中，$θ_ {\ Mathrm {b}} $和$θ_ {\ Mathrm {ng}} $或$θ$或$θ_ {\ $θ_{磁场结构受恒星形成活动的影响。 A statistically more perpendicular alignment is found between $θ_{\mathrm{B}}$ and $θ_{\mathrm{VG}}$ throughout our studied $N_{\mathrm{H_2}}$ range, which indicates a trans-to-sub-Alfvénic state at small scales as well.从极化强度梯度（KTH）方法得出的归一化质量频率比随$ n _ {\ mathrm {h_2}} $增加而增加。
We present ALMA dust polarization and molecular line observations toward 4 clumps (I(N), I, IV, and V) in the massive star-forming region NGC 6334. In conjunction with large-scale dust polarization and molecular line data from JCMT, Planck, and NANTEN2, we make a synergistic analysis of relative orientations between magnetic fields ($θ_{\mathrm{B}}$), column density gradients ($θ_{\mathrm{NG}}$), local gravity ($θ_{\mathrm{LG}}$), and velocity gradients ($θ_{\mathrm{VG}}$) to investigate the multi-scale (from $\sim$30 pc to 0.003 pc) physical properties in NGC 6334. We find that the relative orientation between $θ_{\mathrm{B}}$ and $θ_{\mathrm{NG}}$ changes from statistically more perpendicular to parallel as column density ($N_{\mathrm{H_2}}$) increases, which is a signature of trans-to-sub-Alfvénic turbulence at complex/cloud scales as revealed by previous numerical studies. Because $θ_{\mathrm{NG}}$ and $θ_{\mathrm{LG}}$ are preferentially aligned within the NGC 6334 cloud, we suggest that the more parallel alignment between $θ_{\mathrm{B}}$ and $θ_{\mathrm{NG}}$ at higher $N_{\mathrm{H_2}}$ is because the magnetic field line is dragged by gravity. At even higher $N_{\mathrm{H_2}}$, the angle between $θ_{\mathrm{B}}$ and $θ_{\mathrm{NG}}$ or $θ_{\mathrm{LG}}$ transits back to having no preferred orientation or statistically slightly more perpendicular, suggesting that the magnetic field structure is impacted by star formation activities. A statistically more perpendicular alignment is found between $θ_{\mathrm{B}}$ and $θ_{\mathrm{VG}}$ throughout our studied $N_{\mathrm{H_2}}$ range, which indicates a trans-to-sub-Alfvénic state at small scales as well. The normalised mass-to-flux ratio derived from the polarization-intensity gradient (KTH) method increases with $N_{\mathrm{H_2}}$.
