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The surprising truth about the sun's mass: How do you calculate this incredibly huge number?
In astronomy, the "solar mass" (M☉) is a standard unit of mass, equal to approximately 2×1030 kilograms, a number that is surprising enough. The mass of the sun is not only the basis for measuring the sun itself, but is also often used to describe the mass of other celestial bodies such as stars, star clusters, nebulae, galaxies and black holes. Since the Sun has a mass of about 333,000 times that of Earth, or 1,047 times that of Jupiter, this makes it an important reference point in the universe.
The concept of the Sun's mass predates the precise measurement of the astronomical unit (AU) and the gravitational constant (G).
Measurement History
The history of measuring the mass of the Sun dates back to the 17th century, when Ivy Newton's book "Mathematical Principles of Natural Philosophy" first estimated the ratio of the mass of the Sun to the mass of the Earth. Newton's initial estimate was based on an incorrect value for the daily parallax, which he later revised in the third edition of his work, changing his estimate to 1/169282, and the current value is about 1/332946. .
How to calculate the mass of the Sun?
Since it is impossible to directly measure the mass of the Sun, scientists use other measurable factors for calculations, including the distance from the Earth to the Sun (i.e., astronomical units AU), the Earth's orbital period (about one year), and the gravitational constant G. From this data, scientists used Kepler's third law to deduce the mass of the Sun. Although the measurement of the gravitational constant is very difficult, the standard gravitational parameters of the Sun and several planets have been accurately determined.
The mass of the sun is the standard mass in the astronomical measurement unit system, which facilitates the comparison of the masses of other celestial bodies in the universe.
Changes in the Sun's mass
As time goes by, the mass of the Sun decreases year by year due to nuclear fusion reactions, which is accompanied by the release of electromagnetic energy, neutrinos and matter ejected outward in the solar wind. The Sun is currently losing about 2–3×10−14 M☉ of mass per year. As the Sun enters the red giant phase, this mass loss rate will increase significantly, eventually reaching 10−5 to 10−4 M per year as it forms a planetary nebula. ☉ The peak. Eventually, when the Sun transforms into a white dwarf, it is predicted to lose 46% of its initial mass.
Related Units
One solar mass M☉ can be converted into other mass units, for example: 27068510 ML (Moon mass) and 332946 ME (Earth mass), and 1047.35 MJ (Jupiter mass). In general relativity, mass can also be expressed in units of length or time, specifically M☉ G / c2 and M☉ G / c3.
ConclusionThe use of the parameter of the solar mass (G·M☉) in the astronomical unit laid the foundation for astronomers' understanding of the universe.
Through historical exploration and the development of modern science, our understanding of the mass of the sun continues to deepen. Behind this simple number lies the operating laws and evolution process of the universe. In the future, as technology advances, perhaps we will be able to get a more precise understanding of this important parameter. However, the mass of the sun and its changes undoubtedly remind us how magnificent and complex the laws of the universe are. Have you ever thought about what new mysteries the universe will reveal to us in the future?
