论文标题
惯性力对磁盘星系动力学的影响
The Effects of Inertial Forces on the Dynamics of Disk Galaxies
论文作者
论文摘要
当处理银河系动力学（或更具体地说，使用银河旋转曲线）时，总是采用一个基本假设：相对于旋转速度的参考框架假定为惯性。换句话说，相对于给定星系的观察框架，假定虚拟力消失。但是，探索放弃该假设的结果可能很有趣。也就是说，在观察到的数据中搜索非惯性行为的签名。在这项工作中，我们表明银河旋转曲线的差异可能归因于非惯性效应。我们得出了一个螺旋星系的模型，该模型考虑了虚拟力的可能影响，并发现新模型中的附加术语（由于虚拟力）非常类似于暗光晕谱。遵循此结果，我们将新模型应用于广泛的星系样本，涵盖了大量的亮度和半径。事实证明，新模型可以准确地重现旋转曲线的结构，并为数据提供非常好的配件。
When dealing with galactic dynamics, or more specifically, with galactic rotation curves, one basic assumption is always taken: the frame of reference relative to which the rotational velocities are given is assumed to be inertial. In other words, fictitious forces are assumed to vanish relative to the observational frame of a given galaxy. It might be interesting, however, to explore the outcomes of dropping that assumption; that is, to search for signatures of non-inertial behavior in the observed data. In this work, we show that the very discrepancy in galaxy rotation curves could be attributed to non-inertial effects. We derive a model for spiral galaxies that takes into account the possible influence of fictitious forces and find that the additional terms in the new model, due to fictitious forces, closely resemble dark halo profiles. Following this result, we apply the new model to a wide sample of galaxies, spanning a large range of luminosities and radii. It turns out that the new model accurately reproduces the structures of the rotation curves and provides very good fittings to the data.
