New Solar spectrum figures solve a ten-year-old controversy over the formation of our star.
Although our Sun is very close to any other star in the universe, it still has mysteries. After all, it is still 93 million miles (150 million kilometers) from Earth, and we have very little vision. In addition, its atmosphere is extremely hot its atmosphere is scorching, and it is constantly erupting particles at about a million miles an hour. No wonder we discover new things.
Astronomers have recently solved the problem of a decade of solar eclipse: a conflict between the solar structure as determined by the solar cycle (helioseismology) and a system based on the basic theory of astronomy, which also depends on measurements. of the chemical composition of the modern Sun. New solar physics figures show revised effects of various chemical elements, which resolve conflicts. Remarkably, the Sun contains more oxygen, silicon, and neon than previously thought. The methods used also promise more accurate measurements of the chemical composition of stars in general.
What do you do if the tried-and-true method of determining the chemical composition of the Sun seems to conflict with the new, more accurate way of mapping the solar structure? That was the situation facing astronomers who studied the Sun – until new figures were published by Ekaterina Magg, Maria Bergemann, and her colleagues, and they resolved apparent conflicts.
The pioneering work of the Indian astronomer Meghnad Saha in 1920 linked the strength of those “suction lines” to the temperature of the stars and the chemical composition, which provided the basis for our natural star species. Cecilia Payne-Gaposchkin’s assertion that celebrities such as our Sun contain mainly hydrogen and helium, which have no trace of heavy chemical values, is based on that work.