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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 Kelvin (15 million degrees Celsius; 27 million degrees Fahrenheit). [2]
The coolest layer of the Sun is a temperature minimum region extending to about 500 km above the photosphere, and has a temperature of about 4,100 K. [77] This part of the Sun is cool enough to allow for the existence of simple molecules such as carbon monoxide and water. [81]
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.
Almost all radiation from the sun is emitted from this layer, which has a temperature of 8,100 to 11,000 degrees. Beneath the layer, the hot, dense plasma moved in ways not unlike magma in Earth's ...
This temperature is achieved in the cores of main-sequence stars with at least 1.3 times the mass of the Sun. [32] The Sun itself has a core temperature of about 1.57 × 10 7 K. [33]: 5 As a main-sequence star ages, the core temperature will rise, resulting in a steadily increasing contribution from its CNO cycle. [25]
The temperature at its surface is estimated to be approximately 5,700 K (5,430 °C; 9,800 °F), about the temperature at the surface of the Sun. [5] The inner core is solid at high temperature because of its high pressure, in accordance with the Simon-Glatzel equation. [6]
In the Sun, the frequency ratio of the pep reaction versus the p–p reaction is 1:400. However, the neutrinos released by the pep reaction are far more energetic: while neutrinos produced in the first step of the p–p reaction range in energy up to 0.42 MeV , the pep reaction produces sharp-energy-line neutrinos of 1.44 MeV .
Within that time, the sun oscillates from minimum to maximum solar activity, with maximum activity peaking in the middle of the cycle when the sun's magnetic fields flip. The last solar cycle was ...