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Brown dwarfs: substars without nuclear reactions

机译：褐矮星：没有核反应的子星

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In 1963, Kumar [1] showed that the hydrogen burning in a stellar core stops below some mass limit and the gravitational contraction of the object is balanced by the degenerate electron gas. The equilibrium of thermal pressure and quantum electron pressure implies a limiting mass of ～0.072 solar mass (M_⊙). The limiting mass is somewhat higher, up to ～0.09 M_⊙, for objects in which the heavy element abundance is significantly below the solar value. Substellar objects which are not massive enough to sustain the stable hydrogen burning in the core are called brown dwarfs (BDs). BDs are failed stars. How can one discover such objects? How many of them reside in our Galaxy and how much do they contribute to the hidden mass? Is there a continuous transition from the low-mass substellar objects to giant planets? Do their formation mechanisms differ from ordinary stars? Astronomers have been interested in these and many other questions for several decades.
机译：1963年，Kumar [1]表明，恒星核中燃烧的氢停止在一定质量极限以下，并且物体的重力收缩由简并的电子气平衡。热压和量子电子压力的平衡意味着极限质量为〜0.072太阳质量（M_⊙）。对于重元素丰度显着低于太阳值的物体，极限质量稍高一些，最高为〜0.09M_⊙。不足以维持核心中稳定氢燃烧的亚星体被称为褐矮星（BDs）。 BD是失败的星星。一个人如何发现这样的物体？他们中有多少人居住在我们的银河系中，它们对隐藏物质有多少贡献？从低质量的星下天体到巨型行星是否有持续的过渡？它们的形成机制与普通恒星不同吗？几十年来，天文学家一直对这些问题和许多其他问题感兴趣。

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