photographic magnitude

简明释义

照相星等

英英释义

例句

1.The photographic magnitude scale helps astronomers determine how far away a star is.

摄影星等尺度帮助天文学家确定星星距离的远近。

2.In his research, he focused on the photographic magnitude of variable stars.

在他的研究中，他专注于变星的摄影星等。

3.The photographic magnitude of the supernova was recorded in several different wavelengths.

超新星的摄影星等在几个不同波长中被记录下来。

4.Astronomers often use photographic magnitude to compare the brightness of celestial objects.

天文学家经常使用摄影星等来比较天体的亮度。

5.The telescope was calibrated to measure the photographic magnitude of distant stars.

这台望远镜经过校准，以测量遥远星星的摄影星等。

作文

In the realm of astronomy, the term photographic magnitude refers to a measure of the brightness of celestial objects as captured on photographic plates or films. This concept is crucial for astronomers who rely on photographic techniques to study stars, galaxies, and other astronomical phenomena. The photographic magnitude scale is logarithmic, which means that a difference of 5 magnitudes corresponds to a brightness factor of 100. Thus, a star with a photographic magnitude of 1 is 100 times brighter than a star with a photographic magnitude of 6.The history of photographic magnitude dates back to the 19th century when astronomers began using photography to document their observations. Before this innovation, the brightness of stars was measured using the naked eye, which limited the accuracy and scope of astronomical studies. With the advent of photography, it became possible to capture fainter stars and celestial objects that were previously beyond the reach of human vision. This advancement allowed astronomers to compile more comprehensive catalogs of stars and other celestial bodies.One of the key advantages of using photographic magnitude is its ability to provide a consistent and objective measurement of brightness. Unlike visual observations, which can be influenced by the observer's eyesight and atmospheric conditions, photographs offer a permanent record of an object’s brightness at a specific time. This reliability is particularly important for long-term studies of variable stars, which change in brightness over time. By comparing photographs taken at different intervals, astronomers can analyze these fluctuations and gain insights into the underlying mechanisms driving such changes.Moreover, the use of photographic magnitude has paved the way for significant discoveries in the field of astrophysics. For instance, the identification of new celestial objects, such as supernovae and distant galaxies, often relies on the ability to detect faint light sources through photographic means. The ability to measure photographic magnitude accurately enables astronomers to determine distances to these objects, contributing to our understanding of the universe's expansion and the formation of cosmic structures.As technology has advanced, the methods for measuring photographic magnitude have evolved. Modern digital imaging techniques have largely replaced traditional photographic plates, allowing for even greater precision and sensitivity. Digital sensors can capture a wider range of wavelengths and produce high-resolution images, which enhance our capability to study celestial phenomena in detail. However, the principles of photographic magnitude remain fundamentally unchanged, as astronomers continue to rely on the same logarithmic scale to quantify brightness.In conclusion, the term photographic magnitude is a vital component of astronomical research, providing a standardized method for measuring the brightness of celestial objects. Its historical significance and ongoing relevance highlight the importance of photography in expanding our understanding of the universe. As we continue to develop new technologies and methodologies, the concept of photographic magnitude will undoubtedly remain a cornerstone of astronomical observation and discovery.

在天文学领域，术语photographic magnitude指的是通过摄影底片或胶卷捕捉到的天体亮度的测量。这一概念对依赖摄影技术研究恒星、星系和其他天文现象的天文学家至关重要。photographic magnitude的尺度是对数的，这意味着5个亮度差对应于亮度因子的100。因此，一颗亮度为1的星星比亮度为6的星星亮100倍。photographic magnitude的历史可以追溯到19世纪，当时天文学家开始使用摄影记录他们的观察。在这一创新出现之前，恒星的亮度是用肉眼测量的，这限制了天文研究的准确性和范围。随着摄影技术的出现，捕捉到更暗的恒星和天体成为可能，这些天体在以前超出了人类的视觉范围。这一进展使天文学家能够编制更全面的恒星和其他天体目录。使用photographic magnitude的一个主要优点是它能够提供一致和客观的亮度测量。与视觉观察不同，视觉观察可能会受到观察者的视力和大气条件的影响，而照片则为特定时间对象的亮度提供了永久记录。这种可靠性对于长期研究可变星尤其重要，因为可变星的亮度随时间变化。通过比较在不同时间间隔拍摄的照片，天文学家可以分析这些波动，并深入了解驱动这些变化的潜在机制。此外，使用photographic magnitude为天体物理学领域的重要发现铺平了道路。例如，新的天体（如超新星和遥远星系）的识别通常依赖于通过摄影手段检测微弱光源的能力。准确测量photographic magnitude的能力使天文学家能够确定这些天体的距离，帮助我们理解宇宙的膨胀和宇宙结构的形成。随着技术的进步，测量photographic magnitude的方法也不断发展。现代数字成像技术在很大程度上取代了传统的摄影底片，使我们能够获得更高的精确度和灵敏度。数字传感器可以捕捉更广泛的波长并产生高分辨率图像，这增强了我们详细研究天文现象的能力。然而，photographic magnitude的基本原理仍然没有改变，天文学家继续依赖同样的对数尺度来量化亮度。总之，术语photographic magnitude是天文研究的重要组成部分，为测量天体亮度提供了标准化的方法。它的历史意义和持续相关性突显了摄影在扩展我们对宇宙理解中的重要性。随着我们继续开发新技术和方法，photographic magnitude的概念无疑将继续成为天文观察和发现的基石。