parallax second

简明释义

秒差距

英英释义

例句

1.In astrometry, the concept of parallax seconds is crucial for calculating stellar distances accurately.

在天体测量学中，视差秒的概念对于准确计算恒星距离至关重要。

2.A star with a parallax shift of one arcsecond is located at a distance of about 3.26 light-years, equivalent to one parallax second.

一个视差位移为一个角秒的星星距离大约为3.26光年，相当于一个视差秒。

3.Astronomers often use parallax seconds to determine the distances of celestial objects from Earth.

天文学家常常使用视差秒来确定天体与地球之间的距离。

4.The distance to the nearest star can be measured in parallax seconds, which is a unit of angular measurement based on the apparent shift of the star's position.

到最近的星星的距离可以用视差秒来测量，这是一种基于星星位置的明显变化的角度测量单位。

5.Measuring parallax seconds allows scientists to create a scale for the universe.

测量视差秒使科学家能够为宇宙创建一个尺度。

作文

In the realm of astronomy, understanding distances between celestial bodies is crucial for various scientific endeavors. One of the fundamental concepts used to measure these vast distances is the concept of the parallax second, which is a unit of measurement based on the apparent shift in position of an object when viewed from different angles. The term 'parallax' refers to the phenomenon where the position or direction of an object appears to differ when viewed from different locations. This effect is particularly significant when observing stars and other distant objects in space.To grasp the significance of the parallax second, one must first understand how parallax is measured. Astronomers use a baseline distance, typically the diameter of Earth's orbit around the Sun, which is about 186 million miles or 300 million kilometers. When astronomers observe a star at two different points in Earth’s orbit, they record the star's apparent position against the background of more distant stars. The angle of this apparent shift is known as the parallax angle.The parallax second is defined as the distance at which one astronomical unit (AU) subtends an angle of one arcsecond. An astronomical unit is the average distance from the Earth to the Sun, approximately 93 million miles or 150 million kilometers. Thus, if a star has a parallax angle of one arcsecond, it is located at a distance of one parallax second away from Earth, which is equivalent to about 3.26 light-years.This method of measuring distances using parallax seconds is incredibly useful for determining distances to nearby stars. It allows astronomers to create a three-dimensional map of our galaxy, providing insights into the structure and dynamics of the Milky Way. For instance, the nearest star system, Alpha Centauri, has a parallax of about 0.75 arcseconds, which translates to a distance of approximately 4.24 light-years.Understanding the parallax second also has implications beyond just measuring distances. It plays a critical role in calibrating other distance measurement methods, such as standard candles like Cepheid variable stars. By knowing the distance to these stars through parallax, astronomers can then use them to measure distances to far-off galaxies with greater accuracy.Moreover, the concept of parallax seconds extends beyond astronomy. It can be applied in various fields, including photography and virtual reality, where understanding depth perception is vital. In these areas, parallax effects help create a sense of three-dimensionality, enhancing the viewer's experience.In conclusion, the parallax second is a fundamental concept in astronomy that enables scientists to measure the vast distances between stars and other celestial objects. By utilizing the principles of parallax, astronomers can not only determine how far away these objects are but also gain a deeper understanding of the universe's structure. As technology advances, the precision of measuring parallax seconds continues to improve, allowing for even more remarkable discoveries in the field of astronomy.

在天文学领域，理解天体之间的距离对于各种科学工作至关重要。用于测量这些广阔距离的基本概念之一是视差秒，它是一种基于从不同角度观察物体时位置的明显变化的测量单位。术语“视差”指的是当从不同位置观察物体时，物体的位置或方向似乎有所不同的现象。这种效应在观察星星和其他遥远的空间物体时尤为显著。要理解视差秒的重要性，首先必须了解如何测量视差。天文学家使用一个基线距离，通常是地球绕太阳轨道的直径，大约为1.86亿英里或3亿公里。当天文学家在地球轨道的两个不同点观察一颗星星时，他们记录下星星相对于更遥远的背景星星的明显位置。这个明显移动的角度被称为视差角。视差秒被定义为一天文单位（AU）以一个角秒的角度所对应的距离。天文单位是地球到太阳的平均距离，约为9300万英里或1.5亿公里。因此，如果一颗星星的视差角为一个角秒，那么它距离地球的距离就是一视差秒，大约相当于3.26光年。使用视差秒来测量距离的方法对于确定附近星星的距离非常有用。它使天文学家能够创建我们银河系的三维地图，从而提供对银河结构和动力学的深入见解。例如，最近的星系阿尔法·半人马星系的视差约为0.75角秒，这意味着它的距离大约为4.24光年。理解视差秒也超出了仅仅测量距离的范围。它在其他距离测量方法的校准中起着关键作用，例如标准烛光，如造父变星。通过知道这些星星的视差距离，天文学家可以利用它们更准确地测量遥远星系的距离。此外，视差秒的概念不仅限于天文学。它可以应用于多个领域，包括摄影和虚拟现实，其中理解深度感至关重要。在这些领域，视差效应有助于创造三维感，增强观众的体验。总之，视差秒是天文学中的一个基本概念，使科学家能够测量星星和其他天体之间的巨大距离。通过利用视差原理，天文学家不仅可以确定这些物体的距离，还可以更深入地理解宇宙的结构。随着技术的进步，测量视差秒的精确度不断提高，使得在天文学领域能取得更为显著的发现。