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单词 Solar declination
释义

Solar declination

中文百科

太阳位置 Position of the Sun

(重定向自Solar declination)
在2010年1月3日当地时间上午8:53,从英国拉姆拉什(55° 31'47.43
在一年当中太阳在不同的赤纬时,在天球上路径的变化。此处太阳在夏至和冬至出没的方位角是在纬度56°N观测到的,在地平在线标示的方位以北方为0°。
均时差 —  在轴的上方是日晷显示的时间比钟表的地方平时快的日期,在轴下方是日晷的时间比钟表慢的日期。
The path of the Sun over the celestial sphere through the course of the day for an observer at 56°N latitude.  The Sun's path changes with its declination during the year.  The intersections of the lines with the horizontal axis show azimuths in degrees from North where the Sun rises and sets at the summer and winter solstices.

太阳位置是从地球表面观察时,太阳在天空中的位置,它是时间和地理位置两者的函数。当地球绕着太阳运转一年,太阳似乎相对于在天球上的恒星沿着一条固定的路径移动,这个路径称为黄道。地球自转导致天空中恒星的运动是相对于观测者的地理纬度,沿着一定的路径与方式移动,特定的恒星穿越观测者的子午线的时间与当地的经度有所关联。让一位观测者找到再给定时间的太阳位置,要经过下列三个步骤:

这些计算用在天文学、航海、测量、气象学、气候学、太阳能和日晷的设计都很有用。.

英语百科

Position of the Sun 太阳位置

(重定向自Solar declination)
The Sun seen from Lamlash (55° 31′ 47.43″ N, 5° 05′ 59.77″ W) on 3 January 2010, at 8:53 a.m., local time
The path of the Sun over the celestial sphere through the course of the day for an observer at 56°N latitude.  The Sun's path changes with its declination during the year.  The intersections of the lines with the horizontal axis show azimuths in degrees from North where the Sun rises and sets at the summer and winter solstices.
The equation of time — above the axis a sundial will appear fast relative to a clock showing local mean time, and below the axis a sundial will appear slow.
在一年当中太阳在不同的赤纬时,在天球上路径的变化。此处太阳在夏至和冬至出没的方位角是在纬度56°N观测到的,在地平在线标示的方位以北方为0°。

The position of the Sun in the sky is a function of both time and the geographic coordinates of the observer on the surface of the Earth. As the Earth moves around the Sun during the course of the year, the Sun appears to move with respect to the fixed stars on the celestial sphere, along a path called the "ecliptic". The Earth's rotation about its axis causes the fixed stars to move in the sky in a way that depends on the observer's geographic latitude. The time when a given fixed star crosses the observer's meridian depends on the geographic longitude. To find the Sun's position for a given observer at a given time, one may therefore proceed in three steps:

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