Abstract

Based on Cepheids located near the solar circle, we have determined the Galactocentric distance of the Sun \(R_{0}\) and the Galactic rotation velocity at the solar distance \(V_{0}\). For our analysis we used a sample of \({\sim}\)200 classical Cepheids from the catalogue by Skowron et al. (2019), where the distances to them were determined from the period–luminosity relation. For these stars the proper motions and line-of-sight velocities were taken from the Gaia DR3 catalogue. The values of \(R_{0}\) found lie within the range 7.8–8.3 kpc, depending on the heliocentric distance of the sample stars, on the adopted solar velocity relative to the local standard of rest, and on whether or not the perturbations caused by the Galactic spiral density wave are taken into account. The dispersion of the \(R_{0}\) estimates is \({\sim}\)2 kpc. Similarly, the values of \(V_{0}\) lie within the range 240–270 km s\({}^{-1}\) with a dispersion of the estimates of 70–90 km s\({}^{-1}\). We consider the following estimates to be the final ones: \(R_{0}=8.24\pm 0.20\) kpc and \(V_{0}=268\pm 8\) km s\({}^{-1}\) found by taking into account the perturbations from the Galactic spiral density wave.

中文翻译：

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太阳距太阳圈附近造父变星的银河系中心距离的估计

摘要

根据位于太阳圈附近的造父变星，我们确定了太阳的银心距\(R_{0}\)和太阳距处的银河系自转速度\(V_{0}\)。为了进行分析，我们使用了Skowron 等人目录中的\({\sim}\) 200 个经典造父变星样本。（2019），其中到它们的距离是根据周期-光度关系确定的。对于这些恒星，自行运动和视线速度取自盖亚 DR3 目录。发现的\(R_{0}\)值在 7.8–8.3 kpc 范围内，具体取决于样本恒星的日心距离、相对于当地静止标准所采用的太阳速度以及是否考虑了银河螺旋密度波引起的扰动。\(R_{0}\)估计值的离散度为\({\sim}\) 2 kpc。同样， \(V_{0}\)的值位于 240–270 km s \({}^{-1}\)范围内，估计值的离散度为 70–90 km s \({}^ {-1}\)。我们认为以下估计为最终估计值：\(R_{0}=8.24\pm 0.20\) kpc 和\(V_{0}=268\pm 8\) km s \({}^{-1} \）通过考虑银河螺旋密度波的扰动而发现。