A Drag Dominated Model of the Magellanic Stream
A Drag Dominated Model of the Magellanic Stream
复制标题
麦哲伦流的阻力主导模型
DOI：
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发表时间：
1985
期刊：
影响因子：
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通讯作者：
R. Gingold
中科院分区：
文献类型：
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作者：
G. Meurer;G. Bicknell;R. Gingold
本文介绍麦哲伦流的一系列模型中最好的一个。在这些模型中的主导力是气体阻力。当麦哲伦星系穿过我们银河系周围的热气晕时，气体云从大麦哲伦云和小麦哲伦云之间的桥上撕裂下来。然后，这些小云团被潮汐力和拖曳力彼此拉开，形成麦哲伦流。我们的最佳模型精确地再现了麦哲伦流在天空中的位置和沿着麦哲伦流的径向速度。该协议几乎是最好的纯潮汐模型。在我们最好的模型中，麦哲伦星系与我们的银河系只是松散地结合在一起，并且是第一次与它相遇，这克服了纯潮汐模型的一些问题。我们的一系列模型表明，有一个广泛的参数，将产生一个合理的气流下的气体阻力和重力。
Abstract We present here the best of a series of models of the Magellanic stream. The dominant force in these models is gas drag. Gaseous cloudlets are torn from the bridge between the Large and Small Magellanic Clouds as the Magellanic system passes through a hot gaseous halo about our galaxy. The cloudlets are then stretched apart from each other by tidal and drag forces to form the Magellanic stream. Our best model closely reproduces the position of the stream on the sky and the run of radial velocities along the Magellanic stream. The agreement is almost as good as the best purely tidal model. In our best model the Magellanic system is only loosely bound to our galaxy and is on the first encounter with it. This overcomes some of the problems with purely tidal models. Our series of models indicate that there is a wide range of parameters that will produce a reasonable stream under the forces of gas drag and gravity.