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Deficient Reasoning for Dark Matter in Galaxies

机译:星系中暗物质的推理不足

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In this universe, not all of the matter around us can be readily seen. The further an object is away from us and the less luminous it is, the less visible it becomes. Just by looking at an object is usually difficult, if not impossible, to tell the amount of mass it contains. But astronomers have been using the measured luminosity to estimate the luminous mass of stars, based on empirically established mass-to-light ratio which seems to be only applicable to a special class of stars-the main-sequence stars-with still considerable uncertainties. Another basic tool for astronomers to determine the mass of a system of stars or galaxies comes from the study of their motion, as Newton demonstrated with his law of gravitation, which yields the gravitational mass. Because the luminous mass can at best only represent a portion of the gravitational mass, finding the luminous mass to be different or less than the gravitational mass should not be surprising. Using such an apparent discrepancy as compelling evidence for the so- called dark matter, which has been believed to possess mysterious nonbaryonic properties having a dominant amount in galaxies and the universe, seems to be too far a stretch when seriously examining the facts and uncertainties in the measurement techniques. In our opinion, a galaxy with star type distribution varying from its center to edge may have a mass- to-light ratio varying accordingly. With the thin-disk model computations based on measured rotation curves, we found that most galaxies have a typical mass density profile that peaks at the galactic center and decreases rapidly within ~ 5% of the cut-off radius and then declines nearly exponentially toward the edge. The predicted mass density in the Galactic disk is reasonably within the reported range of that observed in interstellar medium. This leads us to believe that ordinary baryonic matter can be sufficient for supporting the observed galactic rotation curves; speculation of large amount of non-baryonic matter may be based on an ill-conceived discrepancy between gravitational mass and luminous mass which appears to be unjustified.
机译:在这个宇宙中,并不是我们周围的所有事物都能被轻易看到。物体离我们越远,发光越少,可见度就越低。通常,即使不是不可能,仅通过观察物体也很难分辨出物体所包含的质量。但是,天文学家一直在根据经验确定的质光比,使用测得的光度来估算恒星的发光质量,这似乎仅适用于特殊类别的恒星,即主要序列恒星,但仍存在很大的不确定性。牛顿用他的引力定律证明,产生天体引力质量是天文学家确定恒星或星系系统质量的另一个基本工具,是对它们运动的研究。因为发光质量最多只能代表重力质量的一部分,所以发现发光质量与重力质量不同或小于重力质量就不足为奇了。当认真地研究宇宙中的事实和不确定性时,利用这种明显的差异作为令人信服的证据,即所谓的暗物质,被认为具有在银河系和宇宙中占主导地位的神秘的非重子流性质。测量技术。我们认为,星型分布从其中心到边缘变化的星系可能具有相应的质光比。通过基于测得的旋转曲线的薄盘模型计算,我们发现大多数星系都有一个典型的质量密度分布图,该分布图在银河中心达到峰值,并在截止半径的5%范围内迅速下降,然后朝着半径方向呈指数下降。边缘。银河系盘中的预测质量密度合理地在星际介质中观测到的质量范围内。这使我们相信普通的重子物质足以支持观测到的星系旋转曲线。推测大量非重子态物质可能是基于引力质量和发光质量之间的不合理的差异,这似乎是不合理的。

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