Hst/nicmos2 coronagraphic observations of the circumstellar environment of three old pms stars: hd 100546, sao 206462 and mwc 480
Hst/nicmos2 coronagraphic observations of the circumstellar environment of three old pms stars: hd 100546, sao 206462 and mwc 480
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Hst/nicmos2 对三颗古老的经时恒星的星周环境进行日冕观测：hd 100546、sao 206462 和 mwc 480
DOI：
10.1051/0004-6361:20000328
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发表时间：
2000
影响因子：
6.5
通讯作者：
France Canada
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文献类型：
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作者：
J. Augereau;A. Lagrange;D. Mouillet;F. Grenoble;U. J. Fourier;France Canada
由于HST/NICMOS 2相机在$\lambda=1.6 \mu$m的日冕模式，已经观察到了四颗老的主序前星的近距离环境。在该项目的过程中，检测到HD 141569周围的Cir cum stel lar环，并已在Augereau等人（[CITE]B）中提出。本文报道了在Herbig Be星星HD 100546周围探测到的一个椭圆结构，该结构从Co掩模的非常近的边缘（约50 Au）延伸到距离星星350-380 Au（3.5-3.8″）。轴比给出了圆盘相对于视线的倾角为$51\degr\pm3\degr$，位置角为$161\degr\pm5\degr$，从北偏东测量。在50 Au时，盘的表面亮度在10.5和11 mag/arcsec 2之间，然后遵循$-2.92 \pm 0.04$径向幂律直到250-270 Au，最后福尔斯下降为$r^{-5.5\pm0.2}$。推断的光学厚度表明，磁盘是至少边缘光学厚内80 Au和光学薄进一步。结合各向异性散射特性，这可以解释沿沿着圆盘短轴观察到的亮度不对称的形状。这种不对称性需要得到证实。SAO 206462和MWC 480周围的圆星盘没有被解析，导致对灰尘分布的限制。然而，在SAO 206462附近探测到了一个仅相隔0.32\arcsec\pm0.04\arcsec $的紧密双星系统。
The close environment of four old Pre-Main Sequence stars has been observed thanks to the coronagraphic mode of the HST/NICMOS2 camera at $\lambda=1.6 \mu$m. In the course of this program, a cir cum stel lar annulus around HD 141569 was detected and has already been presented in Augereau et al. ([CITE]b). In this paper, we report the detection of an elliptical structure around the Herbig Be star HD 100546 extending from the very close edge of the co mask ( ∼ 50 AU) to 350-380 AU (3.5-3.8″) from the star. The axis ratio gives a disk inclination of $51\degr\pm3\degr$ to the line-of-sight and a position angle of $161\degr\pm5\degr$, measured east of north. At 50 AU, the disk has a surface brightness between 10.5 and 11 mag/arcsec 2 , then follows a $-2.92 \pm 0.04$ radial power law up to 250-270 AU and finally falls as $r^{-5.5\pm0.2}$. The inferred optical thickness suggests that the disk is at least marginally optically thick inside 80 AU and optically thin further out. Combined with anisotropic scattering properties, this could explain the shape of a brightness asymmetry observed along the minor axis of the disk. This asymmetry needs to be confirmed. The cir cum stel lar disks around SAO 206462 and MWC 480 are not resolved, leading to constraints on the dust distribution. A tight binary system separated by only $0.32\arcsec\pm0.04\arcsec$ is nevertheless detected in the close vicinity of SAO 206462.
A.Dogariu：“分形聚合介质反向散射光的增强因子”光学评论。
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伦敦大学学院大盾空间科学实验室/爱丁堡大学（英国）
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