摘要
本文在常数星风速度、稳态质量损失和非球对称的原生星周气体密度分布的假定下,用星风动力学模型研究了双极星云S106的形态结构.结果表明S106的形态可用中央激励星各向异性星风与星周气体的相互作用解释.星风动量驱动的气体壳层的模型还可以很好地解释S106赤道平面中光学和射电发射的缺口以及南瓣中垂直于赤道平面方向上大尺度的类壳层结构.模型导出的中央激励星的质量损失速率_a～(1.3—2.0)×10^(-6)M_☉/年,星风末速度V_*～(160—250)公里/秒以及目前这个气体壳层的位置都与射电、红外等观测结果较好地符合.
To explain the morphology of bipolar nebula S106, we applied the momentum-driven shell model and energy-driven shell model of stellar wind under the assumptions of time independent mass loss, constant wind velocity of exciting stars and exponential decrease of circumstellar material. The results suggested that the structure of S106 is due to the interactions of anisotropic stellar wind with circumstellar gas The gap of optical and radio emissions in the equatorial plan and the shell-like structure at large scale in southern lobe can be explained by momentum-driven model. The parameters derived from the model show the mass loss rate ～(1.3—2.0)*10^(-6)M_⊙/yr, and the wind terminal velocity ～(160—250)km/s of central star. The positions of the shell are in agreement with the observations.
出处
《天文学报》
CSCD
北大核心
1990年第4期324-335,共12页
Acta Astronomica Sinica
