Astronomy

This article focuses on the question of what the next-generation astronomical telescopes will be like, introducing the large aperture of the mosaic mirrors of the world's top-tier astronomical telescopes, the two mainstream models of multiple telescopes working in collaboration and representative devices, and elaborating on the parameter characteristics and development of different types of next-generation astronomical telescopes, including large-aperture mosaic mirrors such as the Thirty Meter Telescope and the European Extremely Large Telescope, multi-mirror collaborative telescopes like the Giant Magellan Telescope, and the LSST telescope, which combines large aperture with wide field of view.

This article explains why giant telescopes need to use active optics and fiber optics technology. It points out that active optics technology can actively overcome the problem of mirror deformation in large-aperture telescopes to improve imaging quality, which is divided into two types: spliced mirror active optics and thin mirror active optics. Fiber optics technology can solve the problem of the burden of large-scale backend instruments and measurement accuracy, and also enable multi-target observation to improve observation efficiency.

This article takes the theme of "Why the starry sky seen by telescopes of different wavebands is different from each other", and explains that since the radiation of celestial bodies is multi-waveband, telescopes of different wavebands can observe different aspects of the same celestial body. Observing with a single waveband is like "a blind man feeling an elephant", and only by combining multi-waveband observations can we gain a comprehensive understanding of celestial bodies.

This article focuses on the topic of why astronomers are so interested in spectroscopy, introduces the definition and research development history of spectroscopy, explains that spectroscopy can be used to analyze the elemental composition, abundance, and ionization state of celestial bodies, study the evolution of stellar structures, the evolution stages of supernova remnants, and the growth stages of protostars, etc. It also mentions that with the advancement of telescopes and spectroscopic equipment, astronomers have been able to conduct full-band spectroscopic observations, and spectroscopy will reveal more mysteries of the universe.

This article focuses on the question of "why do astronomers always take photos of stars?" and introduces the development background of astronomical observation from sketching to photography, the three categories and applications of celestial photos, the analytical basis and methods of celestial photos, the reasons for using photography instead of video recording, and the role of astronomical photography technology in promoting the development of astronomy.

This article focuses on "Why is the bigger the astronomical telescope better", explaining that the larger the aperture of an optical telescope, the more faint and weak light it collects, and its ability is 2 million times that of the human eye; at the same time, according to the laws of optics, the larger the aperture, the ability to distinguish celestial details. The stronger it answers the two major advantages of large-aperture telescopes.

This article focuses on catadioptric telescopes. In the early 20th century, Schmidt designed catadioptric telescopes with special curvature correction lenses. The field of view was large but the lens was difficult to grind; Soviet optician Maksutov switched to a meniscus lens, which was cheaper., widely used in small telescopes. The catadioptric telescope has a large field of view suitable for sky surveys, and there are also many variants used for science popularization.

This paper explains the reasons why most contemporary large telescopes use reflective telescopes: telescopes are divided into two types: refraction and reflection. Refraction has inherent chromatic aberration. When making large apertures, light passes through glass, the requirements are high and the absorption is large. The largest refractive mirror is only 1.02 meters; Reflecting telescopes can be made with large apertures, becoming the mainstream choice for detecting faint and weak celestial bodies.

This article revolves around the controversy over the production of the first astronomical telescope: in 1608, Dutch optician Liebersch accidentally discovered that a lens combination could bring distant objects closer, and made the world's first telescope and reported it to the Dutch government, where he received an order from the Navy; neighbor Jensen claimed that it was invented early but was not announced; in 1609, Galileo improved the telescope for astronomical observations based on this.

This article introduces a variety of celestial bodies that can be observed by amateur astronomical telescopes, such as lunar craters, rings of Saturn, Milky Way constellations, Venus's profit and loss, Jupiter's stripe great red spot, Mars's polar cap, and nebulae and galaxies. It also explains the key points of lens selection, which needs to be combined with observation targets. Select focal length, weigh aperture and portability, and give priority to telescopes with high optical quality, within budget and appropriate aperture, so that the observation efficiency of dim objects can be improved through SLR.

This article introduces that before the invention of telescopes, astronomers relied on classical instruments such as the gustrum, armillary sphere (including the Yuanyou armillary sphere of the Northern Song Dynasty), and Tycho Wall Quadrant. These instruments can measure time and determine celestial coordinates. Among them, the Water Transport Instrument Observatory pioneered the active roof of an observatory and helped Kepler derive the laws of planetary motion.

This article explains that the latitude at which the observer is located determines the rising and falling laws of stars: stars near the north celestial pole at 40° north latitude in the northern hemisphere (such as Beijing) never fall, and stars near the south celestial pole never rise; no visible stars in the north pole fall, stars in the southern hemisphere do not rise, and there is no such phenomenon at the equator. The star trajectory map can visually present this law.