风速垂直分布。格雷厄姆
Wind speed vertical distribution at Mt. Graham
摘要：
风速垂直分布V（h）的特征对于天文站点来说是基本的，原因有很多：（1）风速切变对整个对流层光学湍流的触发有贡献;（2）波前相干时间（τ_0）等一些天文气候参数直接依赖于V（h）;（3）等效风速V_0，控制自适应光学系统必须运行以正常工作的频率取决于风速和光学湍流的垂直分布。此外，靠近地面的风速太强会在望远镜结构中引入振动。在精确压力（200 hPa）下的风速经常被用于检索关于施加到基于自适应光学系统的所有仪器的τ_0和频率限制的指示，但最近证明V_200（200 hPa风速）单独提供关于这一主题的详尽要素是不够的，风速的垂直分布是必要的。在本文中，一个完整的表征的垂直分布的风速强度是在格雷厄姆山（亚利桑那州，美国），网站的大双筒望远镜。利用欧洲中期天气预报中心（ECMWF）的业务分析，我们提供了一个10年以上的气候研究，我们证明这是代表在山风速垂直分布。Graham，除了边界层，我们证明了一个中尺度模式可以提供可靠的夜间估计V（h）以上的天文网站从地面到大气层的顶部（~ 20公里）。
英文摘要：
The characterization of the wind speed vertical distribution V(h) is fundamental for an astronomical site for many different reasons: (1) the wind speed shear contributes to trigger optical turbulence in the whole troposphere, (2) a few of the astroclimatic parameters such as the wavefront coherence time (tau_0) depends directly on V(h), (3) the equivalent velocity V_0, controlling the frequency at which the adaptive optics systems have to run to work properly, depends on the vertical distribution of the wind speed and optical turbulence. Also, a too strong wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning the tau_0 and the frequency limits imposed to all instrumentation based on adaptive optics systems, but more recently it has been proved that V_200 (wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic and that the vertical distribution of the wind speed is necessary. In this paper a complete characterization of the vertical distribution of wind speed strength is done above Mt.Graham (Arizona, US), site of the Large Binocular Telescope. We provide a climatological study extended over 10 years using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF), we prove that this is representative of the wind speed vertical distribution at Mt. Graham with exception of the boundary layer and we prove that a mesoscale model can provide reliable nightly estimates of V(h) above this astronomical site from the ground up to the top of the atmosphere (~ 20 km).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
