We present high spatial resolution spectroscopic measurements of dynamic fibrils (DFs) in the Ca {\small{II}} 8662 Å line. These data show clear Doppler shifts in the identified DFs, which demonstrates that at least a subset of DFs are actual mass motions in the chromosphere. A statistical analysis of 26 DFs reveals a strong and statistically significant correlation between the maximal velocity and the deceleration. The range of the velocities and the decelerations are substantially lower, about a factor two, in our spectroscopic observations compared to the earlier results based on proper motion in narrow band images. There are fundamental differences in the different observational methods; when DFs are observed spectroscopically the measured Doppler shifts are a result of the atmospheric velocity, weighted with the response function to velocity over an extended height. When the proper motion of DFs is observed in narrow band images, the movement of the top of the DF is observed. This point is sharply defined because of the high contrast between the DF and the surroundings. The observational differences between the two methods are examined by several numerical experiments using both numerical simulations and a time series of narrow band H$α$ images. With basis in the simulations we conclude that the lower maximal velocity is explained by the low formation height of the Ca IR line. We conclude that the present observations support the earlier result that DFs are driven by magneto-acoustic shocks exited by convective flows and p-modes.
The solar chromosphere at high resolution with IBIS. I. New insights from the Ca II 854.2 nm line
（节略）目的：在本文中，我们试图确定在Ca II 854.2 nm谱线上进行的成像光谱学作为高分辨率研究太阳色球层的方法的适用性。研究方法：我们利用单色图像获得的干涉二维光谱仪（IBIS）在多个波长内的Ca II 854.2 nm线和几个安静的地区。我们分析了来自窄带单色图像的形态特性和不同的太阳能功能，如网络点，网络间区域和纤维的平均光谱特性。结果如下：来自安静的太阳目标的光谱特性与固定狭缝光谱观测得到的早期结果完全一致，突出了IBIS获得的光谱信息的可靠性。此外，非常窄的IBIS成像清晰地揭示了Ca II 854.2 nm线的双重性质：它的外翼逐渐采样太阳光球，而核心是一个纯粹的色球指示器。后者显示出丰富的精细结构，包括亮点，类似于Ca II H2 V和K2 V晶粒，以及源自甚至最小磁性元素的原纤维。纤维占据了很大一部分的观察视野，即使在安静的地区，并清楚地勾勒出不同的动力学性质的大气体积，强烈依赖于当地的磁拓扑结构。这突出了一个事实，即1-D模型分层沿垂直方向只能提供一个非常有限的代表性的实际色球物理。
Velocity Curve Analysis of the Spectroscopic Binary Stars NSV 223, AB And, V2082 Cyg, HS Her, V918 Her, BV Dra, BW Dra, V2357 Oph, and YZ Cas by the Non-linear Least Squares
High-precision elements of double-lined spectroscopic binaries from combined interferometry and spectroscopy. Application to the beta Cephei star beta Centauri
Chromospheric activity of the double-lined spectroscopic binary BF Lyn
本文介绍了在1996年至1999年的四次观测中对色球活动双星BF Lyn的H_α、H_β、H_α、Ca II H & K和Ca II IRT谱线的同时光谱观测。这两个组分在H_α、Ca Ⅱ H & K和Ca Ⅱ IRT谱线上都有强的发射，应用减谱技术后观察到H_α和H_β谱线的强填充。我们已经发现，热分量（K2 V）总是系统中最活跃的。不同的活动指标的热，冷的组件显示出相关的变化与轨道相位。
THE CANADA-FRANCE REDSHIFT SURVEY III: "Single Emission Line" Objects, Analysis of Repeat Observations, and Spectroscopic Identifications in the 1415+52 and 2215+00 Fields
The KPNO International Spectroscopic Survey. II. H-alpha Selected Survey List 1
KPNO国际光谱巡天（KISS）是一项新的对河外发射线天体的物棱镜巡天。它结合了许多以前的狭缝光谱调查的特点与现代CCD探测器的优势，是第一个纯粹的数字物镜棱镜调查的发射线星系。在这里，我们提出了从我们的红光谱数据中选择的发射线星系候选者的第一个列表，覆盖光谱范围6400至7200埃。在大多数情况下，检测到的发射线是H-α。目前的调查清单涵盖了位于12月（1950年）= 29.5度的一度宽的条带，跨越RA范围12 h 15 m至17 h 0 m。面积62.2平方米度覆盖。共有1128个候选发射线物体被选中列入调查清单（每平方米18.1个）。度）。我们制表精确的坐标和测光每个源，以及估计的红移和发射线通量和等效宽度的基础上测量的数字物镜棱镜光谱。本文利用现有的观测资料研究了KISS发射线星系的性质。
