arXiv 1010.23642010-10-12astro-ph.GA

船底座η星云的三维结构

On the 3D structure of the nebula around η-Carinae

Lorenzo Zaninetti

备注：: 20 pages 10 figures
发表信息：: Published on Advances in Space Research 46 (2010) 1341-1348
DOI：: 10.1016/j.asr.2010.08.018

摘要：

$η$ -船底座（侏儒）周围星云的不对称形状可以用非均匀介质中的球形膨胀来解释。两个模型进行了分析：一个指数和一个逆幂律依赖的密度作为一个函数的距离，从赤道平面。在两极方向存在密度可变的介质，逐渐将原来的球形壳转变为双极星云。在$η$ -船底座周围的星云中，我们知道了自1840年大爆发以来的时间。观测到的半径和速度之间的精确匹配可以通过微调所涉及的参数来获得，例如初始半径、初始速度和表征密度梯度的典型尺度。在球坐标系中，通过引入单方向或多方向的效率，可以将观测到的侏儒半径和速度作为极角的函数与相应的模拟数据进行比较。一旦获得了侏儒的3D空间结构，我们就可以通过沿视线积分来合成图像。为了模拟观测到的图像，我们考虑了一个双极星云具有恒定的厚度和光学薄的发射层。文中还报道了一些相对强度的模拟切割，对天文切割有一定的参考价值。

英文摘要：

The asymmetric shape of the nebula around $η$-Carinae (Homunculus) can be explained by a spherical expansion in a non-homogeneous medium. Two models are analyzed: an exponential and an inverse power law dependence for the density as a function of distance from the equatorial plane. The presence of a medium with variable density along the polar direction progressively converts the original spherical shell into a bipolar nebula. In the case of the nebula around $η$-Carinae, we know the time elapsed since the great outburst in 1840. An exact match between observed radii and velocities can be obtained by fine tuning the parameters involved, such as initial radius, initial velocity and the typical scale that characterizes the gradient in density. The observed radius and velocity of the Homunculus as a function of the polar angle in spherical coordinates can be compared with the corresponding simulated data by introducing the efficiency in a single or multiple directions. Once the 3D spatial structure of the Homunculus is obtained, we can compose the image by integrating along the line of sight. In order to simulate the observed image, we have considered a bipolar nebula with constant thickness and an optically thin emitting layer. Some simulated cuts of the relative intensity are reported and may represent a useful reference for the astronomical cuts.

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英文摘要：

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