When, when moving around the Earth, the Moon falls into the cone of the earth’s shadow, which is cast by the globe illuminated by the Sun, a total lunar eclipse occurs. If only a part of the Moon plunges into the shadow of the Earth, then a partial eclipse occurs. A total lunar eclipse can last about 1.5 to 2 hours. It can be observed from all over the night hemisphere of the Earth, where the moon is above the horizon at the time of the eclipse. Therefore, in any area, full lunar eclipses can be observed much more often than solar ones.
During a total lunar eclipse of the moon, the lunar disk remains visible, but it usually acquires a dark red hue. This phenomenon is explained by the refraction of sunlight in the earth’s atmosphere. Passing through the earth’s atmosphere, the sun’s rays are scattered and refracted. Moreover, mainly short-wave radiation is Continue reading
Traditionally, two main types of landscape — continents and the sea — stand out on the moon. The prevailing shape of the relief of the lunar surface is the lunar seas, which are huge in size basins of dark color. Of course, there is no water in these seas, but so these depressions were named in the distant past for their dark color; these names have survived to this day. Smaller dark spots, by analogy with the seas, received the names of bays, lakes and swamps. The main seas are concentrated within the visible hemisphere. The largest marine formation is the Ocean of Storms. Adjacent to it is the Sea of Rains from the northeast, the Sea of Humidity and the Sea of Clouds from the south. In the eastern half of the disk visible from the earth, a chain stretched from the northwest to the southeast of the Sea of Clarity, the Sea of Tranquility and the Sea of Plenty. The Sea of Nectar adjoins this chain from the south, and the Sea of Crisis from the northeast. Relatively small marine areas are located on the border of the visible and reverse hemispheres. These are the East Sea, the Regional Sea, the Smith Sea and the South Sea. On the reverse side, there Continue reading
Stars whose mass is 1.5-3 times greater than that of the Sun will not be able to stop their compression at the stage of a white dwarf at the end of their lives. Powerful gravitational forces will squeeze them to such a density at which a “neutralization” of the substance takes place: the interaction of electrons with protons will lead to the fact that almost the entire mass of the star will be enclosed in neutrons. A neutron star is formed. The most massive stars can form into neutron stars after they explode like supernovae.
The concept of neutron stars is not new: the first assumption about the possibility of their existence was made by the talented astronomers Fritz Zwicky and Walter Baarde of California in 1934. (A little earlier in 1932, the possibility of the existence of neutron stars was predicted by the famous Soviet scientists L.D. Continue reading