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首页> 外文期刊>The Astrophysical journal >THE HIGH-EXCITATION PLANETARY NEBULA NGC 246: OPTICAL AND NEAR-ULTRAVIOLET OBSERVATIONS AND TWO-DIMENSIONAL NUMERICAL MODELS
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THE HIGH-EXCITATION PLANETARY NEBULA NGC 246: OPTICAL AND NEAR-ULTRAVIOLET OBSERVATIONS AND TWO-DIMENSIONAL NUMERICAL MODELS

机译：高度激发的星云NGC 246：光学和近地微观测和二维数值模型

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摘要

We have imaged the planetary nebula (PN) NGC 246 in the near-ultraviolet wavelengths [Ne Ⅴ] 342.6 nm, the Bowen fluorescence line of O Ⅲ at 344.4 nm, and a nearby line-free region centered on 338.6 nm, as well as Hα, [O Ⅲ] 500.7 nm, and [S Ⅱ] 673.0 and 671.5 nm. Imaging in the 344.4 nm line is necessary to deconvolve contamination of the [Ne Ⅴ] images by O Ⅲ 342.9 nm. The emission from the shell and inner parts of the nebula is detected in [Ne Ⅴ]. The radial profiles of the [Ne Ⅴ] brightness decrease with radius from the exciting star, indicating that the bulk of the emission from this ion is due to the hard UV stellar radiation field, with a (probably) marginal contribution from collisional ioni/ation in a shock between the PN shell and the interstellar medium (ISM). In contrast, the radial profiles of the emission in Ha, [O Ⅲ] 500.7 nm, and [S Ⅱ] are flatter and peak at the location of the shell. The emission of [S Ⅱ] probably traces the interaction of the PN with the ambient ISM. We also present two-dimensional numerical simulations for this PN-ISM interaction. The simulations consider the stellar motion with respect to the ambient ISM, with a velocity of 85 km s~(-1), and include the time evolution of the wind parameters and UV radiation field from the progenitor star.
机译：我们在近紫外波长[NeⅤ] 342.6 nm处成像了行星状星云（PN）NGC 246，在344.4 nm处成像了OⅢ的Bowen荧光线，并在338.6 nm处成像了附近的无线区域，以及Hα，[OⅢ] 500.7 nm和[SⅡ] 673.0和671.5 nm。为了消除OⅢ342.9 nm对[NeⅤ]图像的污染，必须在344.4 nm线成像。在[NeⅤ]中检测到来自星云壳和内部的发射。 [NeⅤ]亮度的径向分布随离激发恒星半径的增加而减小，表明该离子的大部分发射归因于硬UV恒星辐射场，碰撞电离/电离（可能）具有边际贡献在PN壳和星际介质（ISM）之间受到冲击。相反，在Ha，[OⅢ] 500.7 nm和[SⅡ]中发射的径向分布更平坦，并在壳的位置达到峰值。 [SⅡ]的发射可能追踪了PN与周围ISM的相互作用。我们还提出了对此PN-ISM相互作用的二维数值模拟。模拟考虑了相对于环境ISM的恒星运动，其速度为85 km s〜（-1），并包括了风参数的时间演化和来自祖星的紫外线辐射场。

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