HM Sagittae共生系统致密尘埃壳的形态
On the morphology of the compact dust shell in the symbiotic system HM Sagittae
摘要：
人马座HM的共生系统由一颗Mira星和一颗次级白矮星组成。该系统的尘埃含量受到1975年新星爆发的严重影响，该爆发仍在进行中。在中红外操作的光学干涉测量的能力，使我们能够调查目前的几何形状的尘埃信封。我们测试我们以前的光谱干涉研究这个系统与新的干涉配置，增加了紫外线的覆盖范围，使我们能够确定8和13微米之间的源的外观。我们使用VLTI的射电望远镜和单位望远镜（UT）及辅助望远镜（AT），提供PA= 42度至127度的基线。用椭圆高斯模型和球面辐射转移程序DUSTY对数据进行了解释。我们证明，数据可以很好地再现光学厚的尘埃壳的无定形硅酸盐，典型的那些遇到周围的Mira星，其测量的尺寸从8微米增加到13微米。我们确认，包络线是在垂直于二进制轴的方向上更广泛。与我们在以前的研究中所声称的相反，伸长的水平随着波长而增加。更宽的紫外线覆盖范围使我们能够加深我们以前对这个物体的近距离拱星结构的研究。
英文摘要：
The symbiotic system HM Sagittae consists of a Mira star and a secondary White Dwarf component. The dust content of the system was severely affected by the nova outburst in 1975, which is still ongoing. The capabilities of optical interferometry operating in the mid-IR allow us to investigate the current geometry of the dust envelope. We test our previous spectro-interferometric study of this system with new interferometric configurations, increasing the uv coverage and allowing us to ascertain the appearance of the source between 8 and 13micron. We used the MIDI instrument of the VLTI with the unit telescopes (UTs) and auxiliary telescopes (ATs) providing baselines oriented from PA=42degrees to 127 degrees. The data are interpreted by means of an elliptical Gaussian model and the spherical radiative transfer code DUSTY. We demonstrate that the data can be reproduced well by an optically thick dust shell of amorphous silicate, typical of those encountered around Mira stars, whose measured dimension increases from 8 to 13micron. We confirm that the envelope is more extended in a direction perpendicular to the binary axis. The level of elongation increases with wavelength in contrast to our claim in a previous study. The wider uv coverage allows us to deepen our previous investigations of the close circumstellar structure of this object.
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