食双星的四色测光。AD Bootis、HW Canis Majoris、SW Canis Majoris、V636 Centauri、VZ Hydrae和WZ Ophiuchi的XLI紫外光曲线
Four-colour photometry of eclipsing binaries. XLI uvby light curves for AD Bootis, HW Canis Majoris, SW Canis Majoris, V636 Centauri, VZ Hydrae, and WZ Ophiuchi
摘要：
背景：双星的精确质量、半径和丰度的测定为恒星演化提供了重要信息，这是现代天体物理学和宇宙学中心领域的基础。目标：在长期的哥本哈根双星计划中，我们的目标是获得高质量的光变曲线和标准测光，用于确定精确的绝对尺寸和丰度，并与最近的恒星演化模型的结果进行详细比较。方法：在1985年3月至2007年7月期间，我们在位于拉西拉的ESO的Str "omgren自动望远镜上对AD Boo、HW CMA、SW CMa、V636 Cen、VZ Hya和WZ Oph进行了测光观测。研究结果：我们获得了所有6个系统的完整uvby光变曲线、星历表和标准uvby β指数。对于V636 Cen和HW CMa，我们提出了第一个现代光变曲线，而对于AD Boo、SW CMa、VZ Hya和WZ Oph，它们都比早期数据更准确和更完整。由于高的轨道偏心率（e = 0.50），加上低的轨道倾角（i = 84.7），只有一个日食，接近近星点，发生在HW CMa。对于另外两个偏心系统，V636 Cen（e = 0.134）和SW CMa（e = 0.316），已检测到拱点运动，周期分别为5270 +/-335和14900 +/-3600年。
英文摘要：
CONTEXT: Accurate mass, radius, and abundance determinations from binaries provide important information on stellar evolution, fundamental to central fields in modern astrophysics and cosmology. AIMS: Within the long-term Copenhagen Binary Project, we aim to obtain high-quality light curves and standard photometry for double-lined detached eclipsing binaries with late A, F, and G type main-sequence components, needed for the determination of accurate absolute dimensions and abundances, and for detailed comparisons with results from recent stellar evolutionary models. METHODS: Between March 1985 and July 2007, we carried out photometric observations of AD Boo, HW CMA, SW CMa, V636 Cen, VZ Hya, and WZ Oph at the Str"omgren Automatic Telescope at ESO, La Silla. RESULTS: We obtained complete uvby light curves, ephemerides, and standard uvbyβindices for all six systems.For V636 Cen and HW CMa, we present the first modern light curves, whereas for AD Boo, SW CMa, VZ Hya, and WZ Oph, they are both more accurate and more complete than earlier data. Due to a high orbital eccentricity (e = 0.50), combined with a low orbital inclination (i = 84.7), only one eclipse, close to periastron, occurs for HW CMa. For the two other eccentric systems, V636 Cen (e = 0.134) and SW CMa (e = 0.316), apsidal motion has been detected with periods of 5270 +/- 335 and 14900 +/- 3600 years, respectively.
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