Upon careful consideration, the cosmological theory of the origin and structure of the universe begins to crack at the seams.
Take a look at the starry night sky. How did all these countless stars and planets come about? Most modern scientists are likely to answer this question by referring to one version of the Big Bang theory. In accordance with this theory, at first all the matter of the Universe was concentrated at one point and heated to a very high temperature. At some point in time, an explosion of terrifying force occurred. In an expanding cloud of superheated subatomic particles, atoms, stars, galaxies, planets gradually began to Continue reading
Jupiter, the fifth largest in the distance from the Sun and the largest planet in the Solar System, is 5.2 times farther from the Sun than the Earth, and spends almost 12 years in orbit. The equatorial diameter of Jupiter is 142,600 km (11 times the diameter of the Earth). The rotation period of Jupiter is the shortest of all the planets – 9h 50 min 30s at the equator and 9h 55min 40s in the middle latitudes. Thus, Jupiter, like the sun, does not rotate like a solid – the rotation speed is not the same at different latitudes. Due to the fast rotation, this planet has a strong compression at the poles. The mass of Jupiter is equal to 318 Earth masses. The average density is 1.33 g / cm3, which is close to the density of the Sun. The axis of Continue reading
The radio emission of the Sun has two components – constant and variable. During strong solar flares, the radio emission of the Sun increases by a factor of thousands or even millions of times compared with the radio emission of a calm Sun. X-rays come mainly from the upper atmosphere and the corona. Emission is especially strong during years of maximum solar activity. The sun emits not only light, heat and all other types of electromagnetic radiation. It is also a source of a constant stream of particles – corpuscles. Neutrinos, electrons, protons, alpha particles, as well as heavier atomic nuclei make up the corpuscular radiation of the Sun. A significant part of this radiation is a more or less continuous outflow of plasma – the solar wind, which is a continuation of the outer layers of the solar atmosphere – the solar corona. Against the background of this constantly blowing plasma wind, individual regions on the Sun are sources of more directed, amplified, so- Continue reading