為什麼日晷能說明天文學?
日晷把三件事同時編碼進一條影子:時間(小時角)、緯度(盤面的仰角決定影子長短)、軸傾角(夏至與冬至的影子弧相差最多 47°)。「比較模式」讓你在幾秒內看見 15 年教科書圖表無法呈現的直觀。
「時差方程」(Equation of Time)解釋了真太陽時與平均時鐘時間之間每年最多 ±16 分鐘的偏差。成因有二:地球軌道是橢圓(克卜勒第二定律使地球在近日點附近移動較快),以及地球軸傾角(黃道與天球赤道的夾角 23.45°)。兩者疊加後形成一條 8 字形曲線,稱為「日行跡」(analemma)。
本模擬使用水平式日晷(Horizontal Sundial)的簡化模型。實際中,緯度極高的地區(>70°)在極晝期太陽永不下山,影子以螺旋方式繞行,動畫中以特殊提示呈現。赤道附近(<5°)南北半球切換,影子可能越過日晷中心,是正常的天文現象。
Why does a sundial teach astronomy?
A sundial encodes three things in a single shadow: time (the hour angle), latitude (the dial's tilt sets shadow length), and axial tilt (summer and winter solstice arcs diverge by up to 47°). Compare mode makes this visible in seconds — something 15 years of textbook diagrams rarely achieve.
The Equation of Time explains why solar noon can differ from clock noon by up to ±16 minutes across the year. Two causes: Earth's elliptical orbit (Kepler's 2nd law speeds it near perihelion) and the axial tilt (23.45° angle between the ecliptic and celestial equator). Together they trace an analemma — a figure-8 path the sun makes at the same clock time each day.
This simulation uses a horizontal sundial model. At extreme latitudes (>70°) during polar day the sun never sets, so shadows spiral — shown with a status label. Near the equator (<5°), the shadow may cross the dial center (the sun passes overhead), which is astronomically correct.