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The core of the Sun is considered to extend from the center to about 0.2 of the solar radius (139,000 km; 86,000 mi). [1] It is the hottest part of the Sun and of the Solar System. It has a density of 150,000 kg/m 3 (150 g/cm 3) at the center, and a temperature of 15 million kelvins (15 million degrees Celsius; 27 million degrees Fahrenheit). [2]
The core of the Sun extends from the center to about 20–25% of the solar radius. [60] It has a density of up to 150 g/cm 3 [61] [62] (about 150 times the density of water) and a temperature of close to 15.7 million kelvin (K). [62] By contrast, the Sun's surface temperature is about 5800 K.
The minimum temperature required for stellar hydrogen fusion exceeds 10 7 K (10 MK), while the density at the core of the Sun is over 100 g/cm 3. The core is surrounded by the stellar envelope, which transports energy from the core to the stellar atmosphere where it is radiated away into space.
In the Sun, the region between the solar core at 0.2 of the Sun's radius and the outer convection zone at 0.71 of the Sun's radius is referred to as the radiation zone, although the core is also a radiative region. [1] The convection zone and the radiative zone are divided by the tachocline, another part of the Sun.
The Sun, the star in the center of the Solar System to which the Earth is gravitationally bound, is an example of a G-type main-sequence star (G2V type). Each second, the Sun fuses approximately 600 million tons of hydrogen into helium in a process known as the proton–proton chain (4 hydrogens form 1 helium), converting about 4 million tons ...
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The approximate temperature in the solar atmosphere plotted against height. The solar transition region is a region of the Sun's atmosphere between the upper chromosphere and corona. [1] [2] It is important because it is the site of several unrelated but important transitions in the physics of the solar atmosphere:
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