作为暗物质假设检验的通过动力学摩擦在dSph星系中宽双星的紧缩
The tightening of wide binaries in dSph galaxies through dynamical friction as a test of the Dark Matter hypothesis
摘要：
我们估计嵌入在暗物质晕，由于对暗物质粒子的动力学摩擦宽双星的轨道衰变的时间尺度。我们推导出这种衰变的分析标度，并通过广泛使用N体模拟来校准和测试它们，这准确地证实了预测的时间演化。对于密度和速度色散参数推断的暗物质晕的本地dSph星系，我们表明，衰变时标变得短于年龄的dSph恒星人口组成的双星1 $M_{\odot}$星，初始分离大于0.1 pc。这样宽的双星非常显眼，在太阳附近已经被很好地测量过。暗物质假说的预测是，他们现在应该是缺席的恒星星族嵌入在低速色散，高密度暗物质晕，目前推断的本地dSph星系，已经演变成更紧密的双星。在不久的将来，相关的经验测定将在技术上变得可行，并可以提供证据来区分暗物质粒子晕或修改后的引力理论，以解释当地dSph星系中恒星的高色散速度。
英文摘要：
We estimate the timescales for orbital decay of wide binaries embedded within dark matter halos, due to dynamical friction against the dark matter particles. We derive analytical scalings for this decay and calibrate and test them through the extensive use of N-body simulations, which accurately confirm the predicted temporal evolution. For density and velocity dispersion parameters as inferred for the dark matter halos of local dSph galaxies, we show that the decay timescales become shorter than the ages of the dSph stellar populations for binary stars composed of 1 $M_{\odot}$ stars, for initial separations larger than 0.1 pc. Such wide binaries are conspicuous and have been well measured in the solar neighborhood. The prediction of the dark matter hypothesis is that they should now be absent from stellar populations embedded within low velocity dispersion, high density dark mater halos, as currently inferred for the local dSph galaxies, having since evolved into tighter binaries. Relevant empirical determinations of this will become technically feasible in the near future, and could provide evidence to discriminate between dark matter particle halos or modified gravitational theories, to account for the high dispersion velocities measured for stars in local dSph galaxies.
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