          # Solar mass Size and mass of very large stars, from right to left: VY Canis Majoris (17 ± 8 M), Betelgeuse (11.6 ± 5.0 M), Rho Cassiopeiae (14-30 M), and the blue Pistol Star (27.5 M). The concentric ovals indicate the size of Neptune's (blue), Jupiter's (red) and the Earth's (grey) orbits. Properly scaled, the Sun (1 M) only appears as a tiny dot in the center of the ovals (click for higher resolution to see Earth orbit and Sun).

The solar mass (M) is a standard unit of mass in astronomy, equal to approximately 2×1030 kg. It is used to indicate the masses of other stars, as well as clusters, nebulae, and galaxies. It is equal to the mass of the Sun (denoted by the solar symbol ⊙︎). This equates to about two nonillion (short scale) or two quintillion (long scale) kilograms:

M = (1.98847±0.00007)×1030 kg

The above mass is about 332946 times the mass of Earth (M), or 1047 times the mass of Jupiter (MJ).

Because Earth follows an elliptical orbit around the Sun, the solar mass can be computed from the equation for the orbital period of a small body orbiting a central mass. Based upon the length of the year, the distance from Earth to the Sun (an astronomical unit or AU), and the gravitational constant (G), the mass of the Sun is given by:

$M_{\odot }={\frac {4\pi ^{2}\times (1\,\mathrm {AU} )^{3}}{G\times (1\,\mathrm {yr} )^{2}}}$ The value of G is difficult to measure and is only known with limited accuracy in SI units (see Cavendish experiment). The value of G times the mass of an object, called the standard gravitational parameter, is known for the Sun and several planets to much higher accuracy than G alone. As a result, the solar mass is used as the standard mass in the astronomical system of units.

## History

The value of the gravitational constant was first derived from measurements that were made by Henry Cavendish in 1798 with a torsion balance. The value he obtained differs by only 1% from the modern value. The diurnal parallax of the Sun was accurately measured during the transits of Venus in 1761 and 1769, yielding a value of 9″ (9 arcseconds, compared to the present 1976 value of 8.794148). From the value of the diurnal parallax, one can determine the distance to the Sun from the geometry of Earth.

The first person to estimate the mass of the Sun was Isaac Newton. In his work Principia (1687), he estimated that the ratio of the mass of Earth to the Sun was about 1/28 700. Later he determined that his value was based upon a faulty value for the solar parallax, which he had used to estimate the distance to the Sun (1 AU). He corrected his estimated ratio to 1/169 282 in the third edition of the Principia. The current value for the solar parallax is smaller still, yielding an estimated mass ratio of 1/332 946.

As a unit of measurement, the solar mass came into use before the AU and the gravitational constant were precisely measured. This is because the relative mass of another planet in the Solar System or the combined mass of two binary stars can be calculated in units of Solar mass directly from the orbital radius and orbital period of the planet or stars using Kepler's third law, provided that orbital radius is measured in astronomical units and orbital period is measured in years.

The mass of the Sun has been decreasing since the time it formed. This occurs through two processes in nearly equal amounts. First, in the Sun's core, hydrogen is converted into helium through nuclear fusion, in particular the p–p chain, and this reaction converts some mass into energy in the form of gamma ray photons. Most of this energy eventually radiates away from the Sun. Second, high-energy protons and electrons in the atmosphere of the Sun are ejected directly into outer space as the solar wind and coronal mass ejections.

The original mass of the Sun at the time it reached the main sequence remains uncertain. The early Sun had much higher mass-loss rates than at present, and it may have lost anywhere from 1–7% of its natal mass over the course of its main-sequence lifetime. The Sun gains a very small amount of mass through the impact of asteroids and comets. However, as the Sun already contains 99.86% of the Solar System's total mass, these impacts cannot offset the mass lost by radiation and ejection.

Other Languages
Afrikaans: Sonmassa
العربية: كتلة شمسية
asturianu: Masa solar
беларуская: Сонечная маса
беларуская (тарашкевіца)‎: Сонечная маса
български: Слънчева маса
brezhoneg: Tolz Heol
català: Massa solar
Deutsch: Sonnenmasse
Ελληνικά: Ηλιακή μάζα
español: Masa solar
Esperanto: Suna maso
euskara: Eguzki masa
français: Masse solaire
한국어: 태양질량
Bahasa Indonesia: Massa matahari
interlingua: Massa solar
italiano: Massa solare
עברית: מסת שמש
ქართული: მზის მასა
Kiswahili: Masi ya Jua
Lëtzebuergesch: Sonnemass
lietuvių: Saulės masė
magyar: Naptömeg
македонски: Сончева маса
Malagasy: Lanjamasoandro
മലയാളം: സൗരപിണ്ഡം
Bahasa Melayu: Jisim suria
Nederlands: Zonsmassa

norsk: Solmasse
norsk nynorsk: Solmasse
ਪੰਜਾਬੀ: ਸੌਰ ਪੁੰਜ
Plattdüütsch: Sünnmasse
português: Massa solar
română: Masă solară
Scots: Solar mass
sicilianu: Massa sulari
සිංහල: Solar mass
Simple English: Solar mass
slovenčina: Hmotnosť Slnka
slovenščina: Sončeva masa
српски / srpski: Сунчева маса
svenska: Solmassa
українська: Маса Сонця
Volapük: Solamasat
Winaray: Masa solar  